The nautical almanac and astronomical ephemeris for the year ..

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THE

NAUTICAL ALMANAC

AND

ASTRONOMICAL EPHEMERIS

FOR THE YEAR

1834.

PUBLISHED BY ORDER OF

THE LORDS COMMISSIONERS OF THE ADMIRALTY.

London:
PRINTED BY WILLIAM CLOWES, DUKE STREET, LAMBETH;

JOHN MURRAY, ALBEMARLE-STREET.
1833.

PRICE FIVE SHILLINGS,

PREFACE.

‘Tue Navricat Arataxac and Asvnowomtcat, Ermesenas for the Year 1834, has
been constructed in strict conformity with the recommendations of the Astwowomreas
Soctery of Lowpow, as contained in their Report to the Right Honourable the Lords:
Commissioners iepberrer etd a nareescrc rl and will, it is
believed, be found to contain almost every aid that the Navigator and Astronomer can’
require.

‘The several articles contained in this volume are fully explained, and their uses
exemplified, at the ond of the Work, It is only necessary here to state the Tubles
which have been used, and the Methods which have been adopted, in the general exes
cution of the Work. Previously, however, it may not be uninteresting to give a brief
statement of the Origin and Design of the Nautical Almanac, and ite progress up to
the present period.

The Nautical Almanac owes its existence to » Memoria) presented to the Com~
missioners of Longitude, on February 9, 1968, by Dr. Maskeeysx; in which, after
stating many fhets and experiments to prove the utility of the Lunar Method of
obtaining the Longitude at Sea, he concludes, “I fatter mynelf that the frets and
experiments here recited will appear sufGciently vouched to you from the cestifientes
aud testimonies of the gentlemen who have made these trials; and I am authorized by
them to say, that they apprehend that nothing is wanting to make this methed
practicable at Sea but a Nautical Ephemeris,—an assistance which thoy, with many
more, hope for from this Bonrd.’* ‘The Memorial is given at length in“ New and Care
rect Tables of the Motions of the Sun and Moon. By Tostas Maven. To which te
added, the Motheel of finding the Longituele improved. By the same Author. Pab-
lished by order of the Commissioners of Longitude, London, 1770.’* page exvil.

‘The following proceedings, consequent upon this Memorial, are extructed from the:
same Work :—“ At a meeting af the Commissioners, appointed by Acts of Parliament:
for the Discovery of the Longitude at Sea, &e., which was held at the Admiralty, on
Saturday, the 9th of February, 1765,

“ A Maworial from the Rev. Mr. Nevin, Masketyen was read, setting forth to the
effect following, viz, [Here the substance of the Memorial recited.)

“ The following persons, who were attending by Mr. Maskuiyxr's desire, viz.

‘Mr. James Lavnen, Chief Mate of the Egmont,
Mr. Janes Sravumys, late Sixth of the Speaker, Bast Todi Ships,
‘Mr. Ronnnr Scorr, ‘Third Mate of the Speaker,
Mr. Joux Hoxsxtx, Fourth Mate of the Glatton,
‘were then, at his request, called in separately, and examined as to the utility and prace
ticability of the above-mentioned Obvervatiuns : they produced their Journals and some
abstracts of the results of thcir Observations, and all agreed in testifying that they had
eect rina of tl Teeire storm Fray ae Ny ath Seem
a

3
i
a

taken
ns easily and exactly to be male; anit that the Longitude resulting always:
Ee en ae oe Tie ok ae a ae
make the Calculations in a few hours, not exceeding four hours; and
thnt if a Nautical Ephemeris were published, this method might be easily
practised by Seamen.—They then withdrew. ‘The Board, having taken
consideration, came thereupon to the following Resolution, vis, Resolved,
of this Board, upon the Evidence given of the utility of the late
‘ven's Lunar Tables, that it is proper the said ‘Tubles should be printed;
‘application should be made to Parliament for power to give a sum, not |
to the widow of the said Professor, ax a reward for the said Tables,
Bare re Rae Ey bet Set be ea oe
ive a reward to persons to compile a Nautical Ephemeris, and for —
nt the same, when compiled, in order to make the said Lunar Tables of 1
sae

Tn pursuance of this Resolution, Maren’s Widow received a reward of 30000. ;
smd the eclebrated Evirn the sum of 300/., for having furnished the Theorems made
‘use of by Maven in his Theory; and the construction of a Nautical Ephemeris was
‘intrusted to Dr. Masxxnxwn,

‘The first Ephemeria, viz, that for 1767, was published in 1766, since which time ]
the Work has been continued annually. ‘The various Tables which have been emm=
ployed in its construction, up to the period of Dr. Mamnerysn’s death in 1811, are
fully sinted in the following extract from his last Preface, dated Sept. 25, 1810.

“*Mayen’s Tables of the Sun were used in the Computations of the Navricat
Arsuxac, from its first beginning in 1767 to that of 1804, inclusive. From the
Navrican Atxasac of 1767 to that of 1776, both inclusive, or the first ten years,
Maven’s Lunar Tables were made use of. But from the Navricat Acmawac of 1777
to that of 1788, both inclusive, or the next twelve years, the Moon's Place was inserted’
calculated from new Tables, improved from Maver’s Tables, composed by the kate
‘Mr. Cusnuxs Mason, under my direction, from Culculations made by order of the
Board of Longitude upon the Series of Lunar Observations made by the late Dr. Buan-
uy, anil published in the Navricar Atsanac of 1774; in which new Tubles the
Epoch of the Moon's Mean Longitude is 1” lees, that of the Apogee is 56” lees, and’
that of the Ascending Node 45” more than in Maven’s printed Tables, nnd the Equa
tions are calculated to tenths of « second; and moreover one new Equation is intro=
duced, whose argument is the Mean Distance of the Moon from the Sun's Apogee, and.
maximum is 16/4. But from the Nawricat Anaaxac of 1789 to that of 1804, both
inclusive, the Moon's Place wae inserted aa calculated from new Tables still farther
corrected by Mr. Masox, entitled by hin Tastes of 1780, 2 having been completed
about that time, being rendered more exact than the former by the addition of eight
‘Equations to the number in Maven's Tables, taken from Maven’s Theory as to the Arru-
‘menta, but settled as to the Mo.rima from the said Observations, and the whole being
calculated to tenths of a second. However, the 18th Equation of these Tables was not
used, ax it was doubtful whether such an Equation should arise from the Theory of
Gravity, Moreover, the Epochs of the Sun's Longitude in Maven’s Tables, and of the

Uippeninge
ae

Ni
A

* [The British Mariner's Guisle to the Discovery of the Longitule at Sea and Lond, within
Dogret, by Obveewations of the Distance of the Moon fron the Sun and Slars, taken with Bapiar’s
Quadrant, By Dr. Marsuire—S]

PREFACE. ¥

‘Moon’s Longitude and Mean Anomaly contained in Masox’s Tables of 1780, were
diminished at the rate of 10’ in a hundred yeare, reckoned from the year 1756, in the
calculations of the NavrreaAtaumacs foes J"01 to 1804, both nslualre

‘Moon, were
on from Dr. Braotxy’s Catalogue of the year 1760, by subtracting 50”-85 from it, for
each your between 1756 and 1760, to reduce that Catalogue back to the beginning of
1756, und then adding at the rate of 5020 for the Precession of the Equinoxes for
each yeur clapeed after 1756, and applying the Correction of Secular Motion derired.
from the 44th of the folio Tables annexed to the First Volume of my Astronomical
Observations.’*

“ The Calculations of the Planots’ Places were made for the Ermeaunss from 1780*
to 1804 by the Tables contained in the Second Editon of M, Dx ta Lawoe’s Astro~
nomy; und those of the Eclipses of Jupiter's Satellites were made from Mr. Wanoxx-
tiy’s Tables, which make a part of those Tables; excepting the Relipses of Jupiter's
Second Satellite, which were computed from the Ernxsmnis of 1781 to that of 1804,
from new Tubles of Mr. Wancxxrix, published at the end of the Nauricat Aumaxac
of 1779,"

“Tn the year 1792 came out the Third Edition of M. Dr 1.4 Lasnx’s Astronomy,
which he was pleased to make me x present of, containing new Tubles of the Sun,
Means a anc oirh oe slaw oh ABC Re ee ‘These Tables are
constructed upon the best Observations, and upon the Physical Theories of M. 1a
Gnaxon and MI Da ua Prace, founded Coed ies Principles of Gra-
vity. The Tables of the Sun were constructed by M. Desaamnx, entirely from
my observations; the Tables of the Moou are the same with Mr. Cyantes Ma-
sox's Tables of 1780, only substituting M, De 14 Prace’s Acceleration instead of
Marnn’s, and diminishing the Mean Secular Motion by 23’. The Tables of Mercury,
Venus, and Mars were constructed by M. Dr ua Laxpe, The Tables of Jupiter and
Saturn were constructed by M. Dxtammen from the Theory of M. Dx ta Prace, who
has accounted for the great inequalities of their motion to great exactness, The Tables
of the Planet Herschel, called the Georgian Planet by us, were also calculated by M. De~
sannne, according to the method of M. Dx 1a Prace’s Theory of Jupiter and Saturn.
‘The Tables for calculating the Eclipses of Jupiter’s Satellites were constructed by
M, Detasmue upon M. De 1a Prace’s elaborate Theory, and agree with observation
to surprising exactness. The learned world arc much indebted to Mr, Cuanurs
Mason, M. La Guaxon, M. Daa Prace, M. Dr 1a Lanne, and M. Du.asimx, for
these yaluable improvements in the Astronomical Tables, May I flatter mynelf, that T
also have contributed my share to this great work, by directing Mr. Mason in the
improvement of the Lunar Tubles by precise rules, and pointing out to him the Equa~
tions contained in Mayan’s Theory, though omitted in his Tables, to be ascertained
Bnavter's Obrervations, and by supplying a yariety of Observations, from which, in
conjunction with others, this great work bas been completed ?’”

“Tn the year 1806, the French Board of Longitude published further improved
‘Tables of the Sun by M,Dxxastanx; and improved Tables of the Moon by M, BUKo,
founded on M, De 1a Prace’s Theory, with the Maxima of the Equations stated
according to my observations, and the Epochs principally from my observations and
Dr. Braviey’s, In these, besides M. De ta Prace’s other improvements, ix intro-
duced a new Equation of the Moon's Longitude, of the long period of 180 years,

* [Prom 1767 to 1779, both inclusive, De, Hactay’s Planetary Tables were weed —S.]

: marae 5

|
ati |
he states at 14”, but of great consequence in settling the Mean of
‘tho Moon. M. Béxo has introduced six new Equations, in addition to eight Kquas. |

‘xnd our Board of ‘had antici the important use which should be
ererineoniniatoes eins Anataxac” bs)

I was moreover furnished with several copies af the same, by the favour of the
French Board of Longitude. These I fnmedintely put into the hands of our Com~
puters; and the publication of the Navricar and Asrroxomtcar Atatawae for 1813
‘came out, for the first time, distinguished with this considerable improvement.

“The of these Tables having heen adapted to the civil reckoning of time, |
and to the midnight with which the Inst day of the former year ends, and the new one |
‘owins, instead of the noon of the last day of the former year, a# gencrally used in

‘Tables, I tried to adopt this method for the Navrican Atwaxac, but
afterwards thought it best to relinquish it, and to retain the Astronomical Time, fearing
it would be attended with inconvenience, bot in keeping the Register of the Groct=
‘wich Observations, and in puzzling the sailors by changing the method of using the
Navricar Araraxac."

“ The Places of the Planets, and the Times of the Eclipses of Jupiter's Satellines,
inning in the year 1805, have been calculated from the Tables annexed to the
third edition of M. La Laxne’s Astronomy, and the Eclipses of the Satellites set down:
‘to mesn time, instead of apparent time, as formerly.”

“ The Rev. Sasvat. Vixce, Plumian Professor of Astronomy at Cambridge, having
‘had 2n carly communication of the new French Tables, and of the Errata dixcovered im
‘them by the comparer of the Navrtcat Atwaxac and myself, and having aleo noted:
‘several Errata himself, has lately republished them in a neat, elegant, and accurate:

according to Astronomical Time, together with the Tables of the Planets
(taking those of Mars from M, Le Francars La Laxon’s Tables in the Connoisnanee
des Toms of the 12th year,) and the Eclipses of Jupiter's Satellites from the third
edition of M. La Laxpr’s Astronomy. ‘These will be used for the calculations of the
Nacricat Atmawac for succeeding years.’*

“All the Articles of the Epmuarenis were computed by two separnte persons, and
examined by a third, Sac lst ee eed Latitude, Right Ascension, Declix
Sr cept Wy ce pe, nk Whine cnotery end era oa
were corny one ‘i another ; e truth of thee
Calculations esccrtained by means of Differences, whieh, for the Moon's Longitude,
‘were carried &s far as the Fourth Order."

‘The Navrica, Aumanac for the years 1814 to 1820, both inclusive, appears to
hate been compnted entirely from the Tables in the third volume of Professor Vinor's
Astronomy. Burcknanor’s Tables of the Moon, published by the French Board of
‘Longitude af Paris in 1812, were first used instead of Beno's, for the year 1821. In
the 1824, the Eclipses of Jupiter's Satellites were deduced from Drtasmnn’s
pow Tables®, With these two exceptions, Vircr’s Tables continued to be used to the
‘end of the year 1832. :

Tn the Navrican AtwAnac for 1892 are found “Recalculated Elements of Data
snx’s noo Tables for calculating the Eetipsos of Jupiter's Sateltites, by Mr. Huxne

|

z

* Tile tues idea Satellies ite Jupiter; Papréa ts Thiorie de M. te Maryuis de Laplace, ef ba
tials ee faites deguie 1962 juoqu’a Fan 1802, Por M, Danaxone, Paris, 1817,

PREFACE, vii

Ixwiervs,” ax well as «Table of Corrections, founded upon these recalculated Elements,
for the Eclipses of Jupiter's Satellites in the years 1830, 1892, and 1632,
__ The Kelipees of Jupiter's Satellites for 1833 wore computed from Mr, Jaxixixs's

improved epochs, ‘

Vixcn's Solar Tables were used for 1833, but with corrections deduced from Pro-
fessor Army's comparison of Drtamnnx's Tables of the Sun with 1200 observations
made with the new Greenwich Transit, In the Eransnnis for 1832, corrections de-
err oe ihe San shaoy eure Bisa ba sees EEN eee

1832.

Various valuable papers chiefly relating to Nautical Astronomy have from time to time
parle gene jar ali ary aman ea lara a as
under the title of * Selections from the Additions that have been
to the Navrican Aumanac, from its commencement to the yoar 18125” fering
1815,) but with the exception of the introduction of the Apparent Places of 24
principal Stars in the Nautical ALMAxac for 1822, which were increased to 60 in
1827, and Elements for predicting the Occultations of Fixed Stars by the Moon, &c.,
ca eit OF 4 WY acy ev hv poemmemon ba. L. YOY a LABS. Samaras Aree
to have undergone little, if any, variation.

1G the year 1800, reftene wan wiada by the Lonts Ootashiadovets ce the: AissiAliy
to the Astronomical Society, to consider if any, and what, improvements could be made
in the Navttean Atstaxac. The Council presented their Report upon the sabject in
November of the same year, which was immediately approved by their Lordships, and
ordered to be carried into effect for the year 1834. (See page xii.)

‘The present volume, besides a few additions, contains every article recommended in
the Report, excepting only the periods of the Maximum and Minimum of the Light of
the Variable Stars, for which the necessary data could not be

‘The Bphemeris of the Sun Has been computed from Caxsiwi’s Solar Tubles*
Carsuming Greenwich to be 0 36" 45° West of Milan), with Professor Brssn’s
corrections, and the Nutations adopted in the Astronomical Socicty’s Tables, The
computations were made independently for every Mean Noon of the Year.

Cantuxt's Tables are founded on the same Elements as thove of Detasans pub-
lished in 1806, and differ only in their arrangement. Carcaxr assumes for the unit
of cach argument its respective daily motion, and by this arrangement gives consider
able facilities for the construction of an Ephemeris. For the computation of a single
ies ae Sans Ccmiay'e Table: Gemost nTy lE0Qy SSeeeeee, atte ot

Brssea’s corrections of Cartis1’s Tables are given in Nos. 133 and 134 of the
Astronomisehe Nachrichten, We adopts Buxcknannr’s Masses of Venus snd Mars,
which are lees than those of Decasimne, the first in the proportion of 1 to 08875;
the second in the proportion of 1 to 0°95; and a Mass of the Moon =, that of the
Earth, which is lees than that of Detaste, ‘viz. fj, in the proportion of 2 to 0-9:
hence the Equations in Caniini’s Tables IX, XV, and XXVI, require to be each
multiplied by 0°8875; those in Tables XI and XVII by 0-95; and the Equations in
Tables ¥, VI, XIV, and XXV hy 08, according to Bessrx’s rule,

"The true Longitude and Radius Vector thus derived, require to be further cortteted,
on account of Bussxt's new determination of the Elements of the Solar Tables, from a
comparison of his own observations with those of Bravier.

* Exparizione di un nuovo metodo di coxtruire le Tavole Astronomicke Applicato alte Tavole deb Sole.
‘Di Faawcrsco Canuam, Milano, 1810,

#

PREFACE,
he the ' f
Af ¢ denote raiser eer. 80 Gah rections ea

“To the Mean Longitude ob 265 + t,07 144077
eee oe Bees = of 6499 — €,.0°°91015
‘To the Excentricity - - - - - - — 0:0000024625 — ¢..0'00000001 786.
‘The corrections of the J+we Longitude, and Radius Vector, depending upon these
alterations, are of the form a+ bt vedic Oty and thous Volos of the Coacsla
a, b, a’, b’ have been adopted, which are given in Bessus.’s Table LV. ‘
By the advice of Professor Arny, Brssus’s corrections have been adopted in pre~
his own, because they are exhibited in printed Tubles, and can be re>
to; und this principle has been acted upon generally throughout the Work,
having, in-all possible cases, been given to printed authorities.
ae eee Aa ceraed Ties i vies re a
199, and 217 of tho Astronamische Nachrichten.
parent Places of the 100 Stars were directed to be founded upon the N=
inthe Anson Set aby te. ne Naan have been
jun, Moon, aud Planets throughout this Work, in preference to those:
erp aarp amore
The Lunar and Solar Nutations, in Longitude and the Apparent Obliquity of the
Ecliptic, have been deduced from Barix’s Tables XXI and XXU, in the formation
of which the Constants used are those of the Astronomical Society's Tables, CAstra-
nomical Tables and Formule. By Fnaxcis Barux. London, 1827.)
If we denote the several Equations which enter into the Sun's Langitnde, Latitude,
and the Radius Vector, by the numbers of Canuixi’s Tables, the results given in this
Ephemeris, for Mean Noon, are as follow ;

oA

¥

il

the
Ha

Sun’s Longitude ~~ = 11 4-U141V +08 (V-4VI)4VIII +0'8875 (IX) +X
0°95 (XI) 4X11 +Nutations + a6 (t—1800)
Sun's Latitude “8 (XXV) +0'8875 (XAXVI) + XXVIL

Log. Radius Vector = XIIL+0°S (XIV) +0°8875 (XV) + XVI
+095 (XVIT) + XVII + a’+ b° (¢—1800)

‘The Semidinmeter of the Sun, at the Earth's Mean Distance, hos been taken
=16' 0’9, aa determined by Bxssx:,, from 1698 transits, in which both limbs had
heen observed at Konigeberg, between the Years 1820 and 1828, with Reremexnacn’s
meridian circle. (Besse. Tab. Reg. page L.)

‘The Sidereal Time of the Sun's Semidiameter passing the Meridian has been ob-
tained from Tuble XU. of Bussnt's Tab, Reg.

‘The Equatorial Horizontal Parallax of the Sun, at the Earth's Mean Distance, is
= 85776, as deduced by Professor Excxe, frum the Transits of Venus, in 176)
and 1769, (Der Fenusdurchgang von 1769, &c. Gotha, 1824, Page 108.)

‘The Constant af Aberration = 20°36, (Preface to Ast. Soc. Cat. page x.)

Sun's Mean Longitude + Nutations “
‘The Sidereal Time, at Mean Noon = —““* =" “Sues SS. According:

to Drasex (Tab. Reg. page NXIV.), the Mean Longitude of the Sun, at Paris Mean
‘Noon, of January 0* of the year 1800 +f is

279° 54’ 136 4-2. 27605844 +(* , 00001221805 —f’, 14’ 47083,
where f denotes, for the 19th century, the number of years from the preceding bia-
sextile year, Assuming the Meridian of Greenwich to be 9" 21° West of that of
Paris, and altering the epoch to the Mean Noon of January 1 of the year 1800-+2,
the Sun’s Mean Longitude (M) for the meridian of Greenwich is found equal te

PREFACE. = ie

280° 53’ 32°75 + £. 27605844 + . 070001921805 —f. 14’ 47'°083,,
and we havefor the Mean ‘Noon of any day (7) of the year 1800-4,

Sires! Time = 4 n.9° 56555948 + Nutations in R.A.

‘The Mean Obliquity of the Ecliptic hns been tnken = 23° 27" 39-26, for January 1,
1894, and the Mean Annual diminution =0"457. (Busser, Tab. Reg. page 9.)

The Places of the Moon have been derived from Bunexmanut's Tables de la Lune,
(Paris, 1812), with a difference of Meridians = 9" 21", and the Nutations of the
Astronomical Society, They have been computed independently for every Mean Noon:
and Midnight of the Year; and wherever the variation of the Equations appeared to
render such @ correction necessary, second differences have been taken into account,

An Ephemeris of the Moon for the year 1834, calculated upon the Tables of M, Lr

Banox Damorsxav, has been published by Professor Scuemacuen with his Ephemeris —

of Planetary Lunar Distances. Astronomers will thus be enabled to put the merits of
the Tables of Buxcxmannr and Damorskav to the strict test of observation.

Fey Pecetiecbicas a be bel heetacnater Uline ci pcee ‘Saturn,
and the Georgian, have been performed under the direction of Professor Scuvmacnxn,
of Altona; and those for the Minor Planets under the direction of Proftssor Esscrte.

‘The Geocentric, as well as the Heliocentric Positions, are reckoned from the true
Equinox; the former are affected by aberration, and immediately comparable with in-
stramental results, a

‘The Places of Mercury, Venus, and Mare, have been derived from Lrxpexac's
‘Tables* of those Planets, assuning Greenwich to be 42” 56" West of Secbery.

Fupiter, Satum, and the Georgian, have been computed from the new Tables of
Bouvann.t

‘The Semidinmeters of the Planets at the Mean Distance of the Earth from the
Sun, have been usmmed as follow, viz, that of Mercury 8%-23; Venus 8/255
Mars 4-57; Jupiter 93°87; Saturn 86°72; and that of the Georgian 37°20,”

‘The Eclipses of Jupiter's Satellites haye beon computed from Dxrtawnne’s now
‘Tubles, as before, using the corrected epochs given in the Nuuticol Almanac for
1832,

‘The Configurations of the Satellites were deduced from the Tables of Dxrasmee
given in the Conn. des T'ems for 1808, using however, in all cases, ie cere ar:
centric conjunctions and the mean daily motions of the Satellites derived therefrom.

‘The Latitude of the fourth Satellite of Jupiter exceeds. the scmidiameter of the
planet at every conjunction in the year 1834; conrequently the Satellite can neither
be occulted by, nor pass aver the disc of, the planet. When therefore either of these

og ntti reve Orb Biers circa Sogem descripter, accedwat Tubute Planetie ex Elementis
repertes et Thesria Gravifatis Ulwst. De Laplace construct, ductore Benxitaepo Dx Lax.
cee "Gall, 1. sty,

Tabuée Fencris nove et correctic ex Thcoria Gravitalis clurissimi De Laplace et et Observationsbur
receatissimis in apceula Astronomica Seeberyensi habitis erute. Auctore Beunsanvo De Lixonnau,
Goth, 1510, to.

Tabole Martis nove ct correcta e# Theorve Grasiteria clarissimi De Laplace ef ea Oleereotmmibur
recentinimis crue, Auctore Bruraiaxvo De Laxwevav, Riseuberg, 1311. dio

+ Tables Astroncenigues publiées par te Bureau des Longitaites de Brance contenant ley Tobfer he
Jupiter, de Saturne ct a Uranva, constewites opris le Théorie de In Mécheniqne Célester par MA,
Bovyann, Paris, 1821.

‘Occultations and Transits of the Satellites have been computed with ts
‘of the Tables given in the Berlin Ephemeris for 1834. ‘The portion of the pro
by the Dise of Jupiter has been deduced

deduced from the following formule: ‘The Mean Titnes of the Immersion and

i preceding Eclipse being denoted respectively by 1, and E,, and those w
the following Eclipse by I, and Ey.

‘Mean Time of Ingress ohth y atvrection.

‘Mean Time of Egress = BEB 4 correction
motion of some of the principal Bi

cach Satellite, constructed by the late Mr, Hexny Juxnirs.

‘With regard to the Catalogue of the 100 Fixed Stara, the only necessary ad
tion to the explanation given at pages 366, 367, is that the Mean Places furnished
‘Mr. Poxn are the result of his latest determinutions.

‘The Moon-Calmjpating Stars were selected by Mr. Franects Bary,

‘Tho Metn Places of the Stars for this List, as well a» those for the Occultation
have been taken in orier of preference, 1. From the Catalogue of the 100 Stars 4
this Book. 2. From Mr, Poxn’s printed Catalogue of 720 Stars, 3. Fae
Astronomical Society's Catalogue, The reduction of the Mean to the App
Places has been performed by means of the Constanta given in the last Catalogue,

‘The duplicate coraputations of the Elements of Occultations were performed gra=
tuitously by Mr. Mactear of Biguleswade, q

‘The Tides at London Bridge are derived from Tables calculated by Mr. Di
‘under the direction of Mr. Lunnock, These Tables were originally te
mass of Observations made at the London Docks, which Mr. Luwsock has d
ina paper, printed in the Phil, ‘Trane. for 1831, {o this paper Mr. Leauock bh
confined his attention to the Observations made between New and Full Moon
it would appear, from # compariaon of the results deduced from his ‘Tables with
vations made at the London Docks in the months of January, February, and M Z
1832 (Phil. Trans. for 1832), that considerable discrepancies cxisted between the
ee ee ane ‘Mr. Desstov has corrected bis former Tables, by

the results derived from nbout 6000 ailditional Observations with th
results, and theve corrected Tables have been )

Saari Ch Laci’ Of Wlplaco by chereaGoms af tre Polo:Saral
(a Urece Minoris), at any hour of the day, are similar to those published annually by
Professor Scuumacmen, in his Ephemeris of the planetary distances, and are founded |
on the following formule
t=a— pooh + tein)” (prin hy tana
where denotes the Intitude

a the true altitude of the Star
Pp the apparent polar distance, expressed in seconds of arc

hk —— the horary angle of the Star = S—a; 8 being the sidertal time
of observation, and x the right ascension of the Star,

REPORT

vw
‘THE COMMITTEE OF THE ASTRONOMICAL SOCIETY OF
Relative to the Improvement of the Nautical Almanac: adopted by the
November 19, 1880; approved by the Right Honourable the Lords
sioners of the Aduitalty, and ordered by them to be carried into effect,

NAMES OF THE COMMITTEE.
Professor . i

ma Tee, Pee
oe Magi RS. | Her: Dr Meron
NB Those Members, (0 whose annex om arterish is prefired, formed the Sub Commition,

ASTRONOMICAL SOCIETY OF LONDON,
The ork Baa by the Cony Count. hey Asrnonomicat. ay BOCIEES fo to take. nt

REPORT.

Te A Re pe vf
almost ad the results in the Nautical Almanac;

ate 1¢ computations :
Ko. ot then sun at the time of his transit over the meridian,
be computed for the time of apparent noon; but which, by the arrat
ing

to some that @ convenience may ust,
Teverer, that, ‘Soon wore Arspaeninesits this will be = fn ot Th Maly 1o tales
lace, RE ae bre ets ee ces nae nme wes Scat ied, apparent time
‘only mode of dickens Ue could be properly Reset as the seaman had!
ather method of obtaining his time than by observations of the su; nor any other mods
Steareying #100 from day to day then by andinery watches. Other modes, howovers and
now to for obtaining the time; and the great perfection of chronometers and

a

ie

HE
‘t bi

tt :

‘the

red of th «

seaman may be constantly apprized

‘TIME be inserted at the head of

sn he RAN
‘which baw Bown waade.

change

of consideration was of minor

2 The next
‘ture; viz, the
of the cirele.

and of a less nae
‘res 030° In Oe divin

in the arrangement of the

it in most cases more convenient in

a ileatng

Proposal to abolish the use af signs,

ice, the Committee recommend that the use of

i

‘uniform

should be abolished also, and

ia i
‘hat the degrees should in all eases be reckoned from 0 10 360,

aa
i

certain limit ara
them mare in Seite talte oecanenend

Taving

amine

ngements, xppointed ‘x Sub-Committee to, ox:

ines te oa body he
eee:

‘tions which had been forwarded to them, not

only:

ise

ve beet
The

its

in the

une in

ant
28s

Hl

iy
ue jit i
Saati

i

in these

i object for fee hire
perc ip

to remark, that,
princi

view the.

be proper

ke

ir; the
th

of no x

rhaps it mi

ve
ema bee
additional

ins

ei
Hil eid ale

4. And here
the Committee
free was

8 Of |

a
H
&
3
3

the

ee are
ae ue al leuk a
oe

; fon Ha |
a ie i aie unl a

ee je

eH
ae i | cE il H it ult HHT
Hee Te a HH

el
avi :

4 in st iat 3 ps :
38 He < ie =e Bt ES 32 an 4 3
a thi a : ie a in eal i fe

HR ae

ct
As HE UE

ence of
however,
natons,

for the conventer
I
of me

‘the two eolumns entitled “
Nautical Almanac, be
in

with the mean longitu
mend the insertion of the fist

i
:

ee
juation of '

the Committee recommend that,

= FEES é 3
zl ba enreeeeella) é le
| Leal # ue tied ME

| == L ww

‘he
‘oxsthe ;
‘the tenth of a minute, And thet there be also added, at the bottom,

+ vie.

beeration of the sun, the
Of the ecliptic for January Ist ; and the mean daily motion of the moon's node.

al
fscension (in time) :

ES 3

Hi Hult

* Hin Hh i eu ay
| : gizse : ES be
ae
AGG ae
Hitaenele aul
arilansieti! He Hi
festa Get
aiedliide HEle

i Va aa

ani E sty] =

ene ER

ee Ht Uae i
cy Hp 3 Lee

3 ui | 43 a esti

B a i ne
ene i ea
och ans
te iy 3; wal 235. * eee
erethed B taae 3
ae
A ee a
HEHE TEAR]

xviii REPORT.

ie] 5
*y Pogui - [2:3] 6 4] +1414
Auydri- - | 3 | 017] —78 13
* @ Cusiopem 3 | 031] +55 36
A Ceti - | 2:3] 035] 18 55
* 2 Une Min. 2-3] 059] +68 24
ace ~~ | 3 | 116] —9 4 |
= Erdani - 1 | 131] —s8 6 |
+a Aveta — - | 3 | 158] 422 39
7 Ceti - 3 | 234] 4231 ||
eaGeti = - | 23] 253] 4325 |
aren - 2:3] 312] $49 15
«Tauri - - | 3 | 337] +23 34
PRridani - [23] 350] —14 0 |
seta - - {| 1 | 426) +1610 |
SaAuige - 1 | 5 4] +45 49 |
BOrinas- - | 1 | 5 6] — 8 24
B Tau - 2 | 516] +28 97
Orionia- - | 2 | 5 23] — 026
in - | 3-4] 5 25] —17 57
= | 2:3] 5298] — 119
- | 2 | 533] —s4 10 B Draconian - | 2 | 17 97| +52 28
4 Orionis- - | 1 | 546] 4722 | * « Ophiuchi - 2 1797 | +12 43
» Geminorm 3 | 613| 42236 | * y Draconis - | 2 | 17 53| +51 SI
5 | 6 18| +8717 fw Sagitani - | 3-4, 18 4 | —21 6
1 | 620] 52.36 | *3 Ure Min. - | 3 | 18 97 | +86 35
i 1 | 6 98 | —16 29 1 | 18 31 | +38 38
+ Conis Maj. | 2-3| 6 52] —23 45 | - | 3 '18 44) +53 10
3 Geminorum - | 3-4] 7 10 | +22 17 3 18 58| +13 37
3. | 7 24| +32 15 - [3-4] 1917) + 247
12] 730) +539 3 | 19 38 | 410 12
- | 2 | 735} +28 26 - Jie] 1942] + 8 36
3-4! 8 0| 22 49 3-4] 1947 | + 5 69
- | 4 | 833/47 2 - | 3 |2 9] 13 4
3-4| 847 | +48 42 2 | 2012] —57 18
- | 2 | 913] —58 34 - | 1 | 2036] +44 41
2 | 919|— 756 . | 2059] +47
- | 3 | 921] +52 27 - | 3 [21 6| +299
3 | 9 36| +24 33 5 |21 8] +88 4
- | 1 | 959) +72 48 - | 3 [215] +61 8
2 | 10 36 | —38 4B 3 | 2193] — 6 19
- | 1:2] 10 53 | +62 40 - | 3 12126] +69 49
a | M5] +2127 4 23/21 36| +9 6
3 Hyd. et Crat- | 3-4] 11.11 | —13 51 | -| 3 lavs7}—2 8
* penis - | 2-3/ 11 40] +15 31 2 | 2157 | —a7 a7
> Unm Maj. - | 2 [1145 | +5438 | - | 3 | 9233] + 9 57
BChameleontis | 5 | 12 9| 7a 92 | 1 | 9248) —30 1
@Crcis- = | 1 11217] —62 9 | - | 2 | 2256] +14 18
i 23) 12 4 | —22 27 | 45/23 31] + 4 a!
23 | 12 48 | +39 14 - | 3 193 32] +76 4)
1 | 13 16 | —10 16 1; 2 0) +98 0

20. The Committee recommend that the several monthly lists of Phenomena,
given in the first page of each month in the Nautical Almanac, be inserted altogether.
some convenient part of the work: that the conjunctions of the fixed stars with the moa
(as usually given) be wholly discontinued: that the conjunctions in future be confined ty]
the ets with the moon and with such of the fixed stars as may afford any int
results, and to the planets with each other: that such conjunctions be expressed in
ascension (and not in longitude as heretofore), to which should be added the difference
declination to the nearest minute: that the other phenomena which should be noted, be
the times when the planets are in quadrature, conjunction, opposition, perihelion,
lion, and nodes; as well as when stationary and at their greatest elongation and helio,
centric latitude, with the amount of the former expressed to the nearest minute: also thi
time of the sun being in perigee and apogee; the time of the greatest brilianey of Ve
of the maximum and minimum of the flight of Algol and other variable stars, the masim|
‘of the moon's libration, as well as notices of any remarkable phenomena that may be er

18]
ck

ah

He

u

;

LIST OF THE ARTICLES FI SED TO BE ERT
HE Saurical IUMANAG. 7.

articles which are now Introduced for the firvt time (that is, which do not form.
‘the Nautical Almanac or its for 1830, or of the for 1833) are pris
same is to denote the alterations which have been mady in 1

the computations of the other asticlon. By this method, the additions and alterations

readily dintingnistiod. .
arent Aisne te bo abolished in al the eomputaions, eacep in thove foumediabely- eon
peced wa the fn's hu cece nee tomas

‘since Jan. 1st), in nomerical order.
Enumaetal ie the year, sity auch day Ay it
time for every day in the year.
sph sepa dabepelee pap nage
ascension 3
Sun's Bt oh batt ef” S| atte tan
Equation of time (with hourly ferent ice lana, oe ny

PRINCIPAL ARTICLES OF THE CALENDAR,
For the Year 1834.

Golden Number 11 {| Dominical Letter -
Epact = - 20 || Roman Indiction -
Solar Cycle - 23 || Julian Period - -

FIXED anp MOVEABLE FESTIVALS, ANNIVERSARIES,
e. §e.

Epiphany - - , Whit Sunday - - - - May 18
Septuagesima Sunday- - - - ‘Trinity Sunday - - - - - 95
Martyrdom of K. CharlesI. - - Restoration of K. Charles IT.- - 29
Shrove Sunday - - - Feb. 8t. John Bapt.—Midsm' D. June 24
Ash Wednesday - - - - Accession of K. William IV. - -

St, David - - - - - rf Proclamation - - - -

St. Patrick- - - - - ~ Birth of Q. Adelaide -

Palm Sunday - - - - Birth of K. W.IV.* -
Annuneiation—Lady Dey Coronation of K.W.1IV.- Sept,
Good Friday - - - - St. Michael—Michaelmas Day -
EASTER SUNDAY Gunpowder Plot - - Nov.
Low Sunday - - - a Advent Sunday -

St.George- - - - St. Andrew - =

Rogation Sunday - May 4 || St.Thomas - - -

Ascension Day- - - - - 8 || Christmas Day -

© Kept May 28.

‘The Year 5595 of the Jewish Era commences on October 4, 1834,
The Year 1250 of the Mohammedan Era commences on May 9, 1834.

Ramadan (Month of Abstinence observed by the Turks) commences on
January 11, 1834, and on December 31, 1834.

EXPLANATION OF
ASTRONOMICAL SYMBOLS AND ABBREVIATIONS.

°

The Sun. Conjunction.
The Moon. © Quedrature.
Mercury. & Opposition.
Venus. & Ascending Node.

8

N

s.

°

5S wm A

OF

‘The Earth. Descending Node.
Mars. . North.

Vesta. South.

Juno. Degrees.

Pallas. Minutes of Are.
Ceres. Seconds of Are.
Jupiter. Hours.

Saturn. Minutes of Time.
Georgian. Seconds of Time.

co)
Py

KEREE* SP ZOKU e

eR Owe te Ke

LAW TERMS, 1834,
‘As settled by Statute 1 Witt. IV. cap. 70, 8.6. (Passed July 28, 1880.)
Hutary Teru - - - - Begins Jan. 11 Ends Jan. 31
Apr. 15 - - May 8
Trinity May 2200 -«- June 12
Micuaguaas Nov. 3 - - Nov. 25

For Returns see Statute 1 Witt. IV. cap. 3, sec. 2. (Passed Dec. 23, 1830.)

UNIVERSITY TERMS, 1834.

Oxrorp. CamprincE.
Names. =
Begin, | Ends. Begins. | Divides. Ends,
Hilary - - | Jan. 14 | Mar. 22] Jan, 13 | Feb. 15, Midnight. | Mar. 22
Eester - - | April 9} May 17] April 9| Mey 22, Noon, | July #
tnt = = | Bog et Taig ae Sa ofa gee em

Michaelmas - | Oct. 10 | Dec. 17] Oct. 10 | Nov. 12, Midnight. | Dec. 1&

The Commencement, July 1

EPHEMERIS

FOR THE YEAR
1834,
FOR THE MERIDIAN

oY THE

ROYAL OBSERVATORY AT GREENWICH.

Absa
1b 008

10-992
10-979
Lo-9as

12 51°16] 10-924
17 13-58] Logit
i) 21 35 45) 10-890

10-265
10-440
lola

lo-ns7
14] 19 48 16717] 10-759
10-730

10-700
17}19 56 8°68} 10-670
18/20 0 24°75) tobe

4 40-06) 10-606
8 54°61) 10-574
13° 6°39] 1o-s4e

17 21°39] 10°09
21 88°60] 10475
25 45°00! 10-442

29 55°62) 10-409
34 5743) 10-378
38 14°43) los

42 22-62) 10-s08
| 46 30-02) 10-274
| Thur. 30/20 50 36-60] 10-240
}) Eid, |91]20 54 42°38] 10-208

32]20 58 47°34

.
iioae fs

S17 8 41°2

rr

RE SAR ANN Leuy

S32 ase a5.

sod Ges Ss

Be wee
2S aes

* Mean time of the Semidiameter passing may be found by subtracting O19 fom the Siiteres

Amys or tne Week.
Days of the Month,

REE

pat

19 12 49°97
1917 12-31
19 21 84-11

5R2

=

19 25 55°39
19 80 16-10
19 34 36-20

19 38 35°67
19 43 lag
19 47 32°64

19 51 50°09
19 56 6°88
20 0 29-95

a

20 4 $810
20 8 S261
20:13 6°34

20 17 19°30
20 21 3147
20 25 42°84

20 29 S34e
20.34 3°20
20 38 12°18,

S88 288

20 42 20°34
20 46 27°71
20 50 84°27
20 54 40°03

£233

20 34 505

20 22 27°5
20 9 416
1g 56 33-0

20.59 44°98 | S17 8 Sat

16 8

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BES S22 £88 a

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12 995
12 2436

12 38-39
12 51°81
13° 4°24

13 15-54
13 26-65
13 36°66
13 45°86

13 54°26

18 43 376 i
18) 46 34702
18 50 30°58

18 64 27°13
18 58 23-69

19 6 16°81
19 10 18°36
19 14 9-92

19 18 648
19 22 3/04
1g 25 59°39

19 29 5613
19 83-52-71
19 87

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S88 888 sss
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JANUARY,

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4 927-4] 242/20 12-0 |

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| Sun. | 12] $20 35 47 -2/326 38 12-8

[19] 44.35 44+
20] 57 11 35

Sat.

6 JANUARY, 1834.

WEDNESDAY L, 4
50 35 °53|N.6 40 53-1 0 13 34
1/13 36
2/13 38
5 3/13 40
5 4/13 42
5 5/13 44
12 3 46°58) 5 18 28-4)ise23 |] 6 | 13 47
We 55765) 5 4 39-Ifaseus | 7/18 49
12 8 8-97| 4.50 48-4)iss-64] 8/13 51
12 10 19°93] 4 36 S6-Sliseess | 9 [13 53
4 10/13 55
4 11/13 57
3 12 13 59
3 isjl4 2
12 21 12-69] 3 27 Be-1}ia9-56 |} aa da 4
j12 23 22-85) 3 13 24-B)is9-~47 ] 15 [14 6
12 25 32°89] 2 59 26-8]139-76 | 16 |1d 8
jie 27 a2-m1) 2 45 28-2}isy-xa | 17 [14 10
12 29 52-62] 2 31 29-Blis9-91 | 18 |1d 12
12 32 2-32] 217 29-7/199-96 | 19 | 14 14
[12 34 11-92] 2 3 30°O/140-00 | 20 [14 17
12 36 21-42] 1 49 29 -Q]140-03 | 21 | 14 19
12 38 80°82] 1 35 29-7/140-05 | 22 |14 21
{a2 40 40°13]N.1 21 29-4}140-05 | 23 114 93
AY
12 42 49 -34|N. 7 29-1 |iso-os | O14 25
12 44 58°47 53 ge-s|iso-os | 1 [ta 97
1247 7°53 39 28°6/1s9-99 | 2/14 30
12 49 16°51 25 28-7/1s9-95 | A [14 32
12 51 25°42)N.0 11 29 O)1s9-%9 | 4 ta SH
12 53 34°26/S, 2 30°3}1s9-81 | 5 ]14 36
12 55 43-08 16 29-2)1a9-79 | 6 14 88
1257 51°74 30 27-6|189-63 | 7
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THE MOON'S RIGHT ASCENSION AND DECLINATION, !

i

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bom " or
435 3 pee] o #3 23 416
437 4) yes]. 23.24.53%
440 4°32 419 59 9% 2/637 8 23 25 539)
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4.46 58°97) 20 20 20-4 $ | 644 51:12) 23 28 34
449 17°33, 20 27 186 6| 647 25°65| 23 28 209
451 37-04 20 33 564 7 | 650 0-98] 23 28 40-2)
453.5092) 20 40 348 8/652 95°20) 23 28 490
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CONFIGURATIONS OF THE SATELLITES OF JUPITER.
At 7", Mzaw Time.

Apparent Eaat,

‘This Table represents, at 7 after Mean Noon of each day of the month, the relative positions:

} Jupiter and his Satellites, ax they woull appear (disregarding their latitudes) in the focus of a tele.
seope that inverts objects, Jupiter is indicated by the white eirelex (O) in the centro of the page
—tha Satellites by poitts. The numerals 1, 2 3, or 4, annexed to the points, serve to disti
the Satolltes from esch other; and their positions are mich as to indieate the directions of the Satel|
Lites motions, which are in all cases tu be coasidered as ¢nwards the numerats, When a Satellite
‘at its greatest elongation, the point is placed above or below the ecutre of the numeral, A whil
circle (©) at tho left or right hand of the page, denotes that the Satellite placed by the vide of it ie
‘on tho dise of Jupiter, and a blsek circle (@) that it Is either behind the dise, or in the shadow, of
Jupiter,

JANUARY, 1834.

APPROXIMATE SIDEREAL TIME

oy rite
OCCULTATIONS OF JUPITER'S SATELLITES BY JUPITER,
4xo oF KE |

TRANSITS OF THE SATELLITES AND THEIR SHADOWS
OVER THE DISG OF THE PLANET.

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FEBRUARY, 1834. iG
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a@ Aquila E. 9
Mars E. 40
Sun E, [tog 58 24/2711 107 21 5yl2729]t05 45 58!

CONFIGURATIONS OF THE SATELLITES OF

At 8", Mean Trae,

oe
*
fe}te)

‘aaa
| 1 |
| 2 |
ro |
|_ 4 |
|_ 5 |
| 6 |
i
| 9 |
|_t0 |
ja |
| 12 |
| 13 |
[13 |
|_15_|
|_16 "|
[17]
| 18 |
Far

esaee

Circle (0) at the left or right hand ofthe page, denctes that the Satalito placed by the side of fe
fn the dive of Supiter, and o black isla (() that iin cither behind the dis, or tthe dang
Supiter.

x. FEBRUARY, 1834. 43

ECLIPSES OF THE SATELLITES OF JUPITER.

larmcane Dag of th

a
1 | at 0
: a | 16 ; 13 22 10°
de | 10 55 738 772
7 Ea 234 8°3
8 | 93 53 ‘l

oe

=
= -
SESSRSESES
feed

BSS=

44 FEBRUARY, 1334,

: ov rine
OCCULTATIONS OF JUPITER'S SATELLITES BY
any of THE

TRANSITS OF THE SATELLITES AND THEIR SILADOWS
OVER THK DisC OF THE PLANET.

SSeScokBssks
Bercuoews.
vous.

eusne
OERSSnSa8s

FEBRUARY, 1834.

|—9'3678 |+9°7731
9'3626 | 9-7524
9°3574

E19
P10 | 11676
1-1i89 | 1 *1601

11265 | 41-1594
11339 | L144
T1410 | 171360

171478
11544
1°1608

i—9 3522

+1-1274
11185
11093

+1°0997

+9 5367
9°3157 | 95010
9-464

+9 4204
93000 | 9°3743
59-3233

+1 70343
1-2039 | 10218
10089

$0"9954
12169 | O"98t4
12209) 0°9668

+9 '2660
92813 | 92011
51256

+9 0355

12247 | 40-9516 +8 5551
19284 | 0°9356 | 92528 |+-8 0934
18319 | 0°9190 —$ ‘0253

+0°9015
12383 | 08932
1241s | 0-639
08436

85198
gr2370 | 87419
9-2317 | 88848

“2263 | 89903

90734

28 27°78
24 31°87

+0 8222

Sut. 798 481

| Sur, gas 59'1

Mon, 53 38

Tues, 630 27

Wed. 6 6560

Thur, 543 42 11 3340
| Fea. 5 20 27°8 11 19-04
Sat. 457 7°0 11 4°28)
| Sun. 433 42°3 10 49°15
Mon. 40 M1 10 33°69
"Putes, $46 42°9 10 17786
Wed. 323 89 10 17R
Thur 259 325 9 45°26
}| Frid. 2 85 643 9 28

| Sat, 2124 9 11°30.
|

} Sun. 148 33°6 § 54-22
| Mon. lag 8 3672)
} Pues.) 11 9% 8 19°08
| Wed. 0 37 27'5 46) 8 1

} Thur, S.0 4 46"1 aa] 7 aval
| Frid. 0 9 55°0 vag] 7 24°78
|

} Sat. 5 0 98 35-0 4-41 i Gta
}} Sun. 8 057 18°6 arsg 47-95
| Mon, 12 120 90° 4°38] 6 29-42
} Tues, 14a 1 4°38] 6 10-82
Wed. 27 aes] 5 5297
Neal 2 4°37] 5 83°55,
}) Frid, | 28 3 1 438) 5 lao
Sat. | 29) 8 1 4°38] 4 56-34
1) Sun. | 30 3 1 4-39] 4 37°80
Mon. | 31} 0 37 50°89 44520] 57-9611 440] 4 19°35
Tues) $2) 0 41 29°05 428 370 1 4-42) 4 1-01

i

‘Time of the Semidiameter passing may be found by yubtracting 0-18 ftom the Sidereas Tim

home
22 47 53°09

ou bm ]
7 % 22.35 14-24

22 51 37°49 i 161 vz 39 10°80
22 55 21°43 531 16 8 2243 7°35 ||
259 4°90 6 30 14° | 16 84 22 47 3-90 |]
23 2 47°91 6 7 74) 16 81 22 51 0°46 |]
23 6 30-58 543 554 | 16 79 a2 54 57°01 |]
23 10 12°71 5 20 3R°8 | 16 7G) 11 Ig'i5 | 22 5H 53°56
23°13 54°51 457:17°8|16 73) tt 439] 23 2 sone |
28:17 35°94 433 52-9| 16 7-1) 10 49°27] 23 6 46°67
28 21 17-02 410 24°51 16 6-8] 10 33-80 | 23 10 43-22

846 53°0 | 16 65] 10 17°97 |} 23 14 eel

323 18°7| 16 6-3] 10 1°82] 23 18 36433
28 32 18°25 259 4271] 16 6-0] 9 45°37 | 23 22 82-88
23 85 58°06 236 3°6|16 58] 9 28°68 | 23 26 e949
28 39 37°60 212235 | 16 55] 9 11°61 | 23 30 25°99
28 43 16°87 148 424/16 5-2 23 34
23 46 55°98 125 04/16 5-0 83 38
23 50 34°75 11180] 16 47

23 54 13°39 037 35-7) 16 4%
23:57 51°85 |S. 0 13 53-7 | 16 42
0 130417|N.0 9477/16 3-9
0 5 8°37 0.93 28°70) 16 36
0 8 4615 057 69) 16 3-3
0 12 24446 120 44°1 | 16 371
016 2741 144 19°2 | 16 2-8
9 40°32 2 751%) 16 25
0 93 18"2t 231 218] 16 2-2
o 2 “99
0 3 “40
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0 at esas | N. 427 591 | 16 0-8

‘Semidiarneter for

Apparent Noon may be assumed the same as that for Mean Noon.

99972235

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9 48°98/S.19 47 3671
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23 21 2971
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THURSDAY 6. SATURDAY 8.
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64: MARCH, 1834. x

CONFIGURATIONS OF THE SATELLITES OF JUPITER
At 8*, Mean Tie.
Days
gite Apparent West, Apparent East,
TOs
E Oo 1 ®
“3 re O
4 32 [e) By
a1 40 3 2
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‘This Table represents, at 8 after Mean Noon of each day of the month, the relative positios
‘Topiter and his Satellites, as they would appear (disregarding their latitudes) in the focus of a
seope that inverts objects. Jupiter is indicated by the white circles (©) in the centre of the p
—tho Satellites by points. The numerals 1, 2, 3, or 4, annexed to the points, serve to disting
‘the Satellites from each other ; and their positions are such as to indicate the directions of the §
lites motions, ~which are in all cases tu be considered as fowards the numerals. When a Satelli
at its greatest elongation, the point is placed above or below the centre of the numeral. A w
cirele (0) at the left‘or right hand of the page, deuotes that the Satelite placed by the side of
‘on the disc of Jupiteryand a black circle (@) that it is either behind the disc, or in the shadow
Sopiter. =

x. MARCH, 1834. 65

ECLIPSES OF THE SATELLITES OF JUPITER.

PHASES

Days of the!
‘as seen in a Telescope that inverts,

Meath, | Mean Time, | Sidereal Time.

“

homo »

I. 2 | 541 266
4 | 010255
5 | 18 39 19°7
7 [13 8 188
9* | 737 12:7}
a 2 6108
12 | 2035 4:3
wo} is 4 155
16 | 9 32 54-0
1s | 4 150-9
19 | 22 30 42°83
21 | 16 59 38:9
23 | 11 28 30:3
25 | 5 57 25-4
27 | 0 2615-9
28 | 18 55 10°6
30 | 13 24 0-3

I. 1 }1119 40
5 0 36 576
8 } 13 545071
12 | 3 12 436
15 | 16 30 38°9
19 | 5 48 317
22 119 627°5
26% | 8 24 23-9

eeissade

66 MARCH, 18384. x

APPROXIMATE SIDEREAL TIME

ov Tue

OCCULTATIONS OF JUPITER'S SATELLITES BY JUPITER,

ann ov Tamm

TRANSITS OF THE SATELLITES AND THEIR SHADOWS
OVER THE DISC OF THE PLANET.

Ocuuerarions, ‘Taanurrs o7 Sareiisres. ‘Taanarrs or Sean

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$5 da-00

* The Semidiameter for Apparent Noon may be aswurved the same as that for Mean Noon,

APRIL, 1834,

74
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AU’ 40", Maan Taste,

‘Tue SATELLITES oy JUPITER

are not visible
from the 10th day of April until the 7th day of June,

JUPITER being too near to the SUN,

‘This Table represents, at 7° 40% afer Mean Noon of each day, the relative positions of Ju
} and hix Satwilites, as they would appear (disregarding their latitudes) ia the focus of w
scope that inverts objects. Jupiter is indieated bry the white circles (©) in the cent of the jy
—the Ssicllitus by points. ‘The numerals I, ¥, 3, or4, annexed to the poiuty, serve to disting
the Satellites from cack other anit ther potions are such as to indicaty the dirvetions of the §
tites motions, whieh aro in all cases to. be considered as fowarde (Ae numerals, When « Satelli
‘tits greatest clongation, the point is placed above or below the centre of the numeral, AW
éirelo (©) at tho loft or right hand Of the page, denotes that the Satelite placed by tbe side of
om tho dise of Jupiter, and a black circle (@) that itis cither behind the dise, or in the shadoy

x. APRIL, 1834, 87

ECLIPSES OF THE SATELLITES OF JUPITER.

[Days of the] PHASES
rare etn | Mean Time. | Siderea! Time, ‘as soon in a Telescope that inverts.
hms
IL le | 7 52 54-2
3 221 43°3
4 | 20 50 36°6
6 15 19 24-4
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Tue ECLIPSES or raz SATELLITES or JUPITER
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from the 10th day of April until the 7th day of June,

JUPITER being too néar to the SUN.

APRIL, 1834. xx

APPROXIMATE SIDEREAL TIME
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OCCULTATIONS OF JUPITER'S SATELLITES BY JUPITER,
AnD OF TEE

TRANSITS OF THE SATELLITES AND THEIR SHADQWS
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are not visible

from the 10th day of April until the 7th day of June,

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"MEAN TIME. _
THE MOON'S RIGHT ASCENSION AND DECLINATION.

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CONFIGURATIONS OF THE SATELLITES OF JUPITE:

Taz SATELLITES or JUPITER

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‘Tus, ECLIPSES or tut SATELLITES or JUPITER

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116 MAY, 1884. 3

‘APPROXIMATE SIDEREAL TIME

ov Tax 3
OCCULTATIONS OF JUPITER'S SATELLITES BY JUPITER,
AND Ov THE

TRANSITS OF THE SATELLITES AND THEIR SHADOWS
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‘Days of the Month.”

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15 35 12°11
15 37 33°20
15 39 54°51
15 42 16-04
15 44 37 80
15 46 59°7

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THE MOON'S RIGHT ASCENSION AND DECLINATION,
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SATURDAY 28.
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XII. JUNE, 1834, 128

MEAN TIME.

Right Ascension.| Declination,
MONDAY | 30.

12190
191-90
12190
191 89
11 5

191-86 r 5

12183 6

191-80 ‘ 6 13 20°3
191-76 i 6 25 152
1-78 ‘

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PHASES OF THE MOON.

ab om
@ New Moon....... esieiseshciais ORE M4
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MEAN TIME.
LUNAR DISTANCES,

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32 12 Ad}2a16] 33 58 20
68 38 54} xs09] 66 53 7)

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CONFIGURATIONS OF THE SATELLITES OF J

At 14" 30", Maan Troe,

‘The SATELLITES are not visible until the 7th day of this month, —
JUPITER being too near to the SUN.

felted fertelKel eral eyfettefefeyoy(e)
al? ces Oe cd

Al

{e}(e)}(e}(e}(e)(e)(e}(e)

]] ‘This Tablo represents, at 14° 30" after Mean Noon of each day, the relative posti
Tuyiter and his Satellites, us they would appear (diseeganting thele latitudes) in the focus of
scope that inverts objects. Inpiter is indicated by tho white circles (O) in the centre of
—tha Satullites by points. ‘Fhe numerals 1, 2, 3, or 4, annexed to the points, serve to
the Satullites from each other ¢ and their positions sre such as to indicate the directions of thi
j| lites motions, which are ia all cases to be considered ax fowarste the numerals, When a
] ot its greatest elongation, the point is placed above or below the centre of the sumerml.
circle (©) at the left or right ha: U of the page, denotes that the Satellite placoit
pobre Lele ae circle (@) that it is either behind the disc, or in the
iter,

'¢ JUNE, 1834... rr

PHASES

suzrra|Days of the’ Mean Time, | Sidereal Time.

Month, ‘as seen in a Telescope that inverts.
hom
I. 7 | 11 56 57-4
9 | 625 s1°0

1. 8 | 21 27 4271
12 | 10 46 16°7
16 | 0 4 16-7

Il. 13 | 13 30 37-0

* The Satellites are not visible until the 71h day of this Month,
Jupiter being too near to the Sun,

ae

APPROXIMATE SIDEREAL TIME
ov Tne
OCCULTATIONS OF JUPITER'S SATELLITES * BY J
Axo ov THK

‘TRANSITS OF TAE SATELLITES AND THEIR SHADOWS
OVER THE DISC OF THE PLANET.

* The Satellites ore not visible until the 7th doy of this Month,
Jupiter being too near to the Sun.

For correcting the Places of the Fixed Stark | Mfesn ‘Time i

*~ At Mean Midnight,
Logaritha of

—0°7856 |—1 "2843 | +8 744
O-7641 | 172867 | 8-701
0°7412 | 172890] 8°7947

077170 |—1 2912 | 4-8 '8182
O-Ogi2 | L-2gaz | 878405
06637 | 12951} 88618

—0 6342 |—1 "2969 |+8 ‘S822
06025 | 12986] $9017
0-568] | 13001] 89205

—0 5306 |—1 "3015 | +8 "9385 18 43 29°18
OnSo4 | 13088] 8 'Y559 18 89 33-2
O-4438 | 1": 89726 18 35 37S

—0 “3928 " +8 ‘9888
0-3g48 | 15 90044
02677 . 90195

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0 0908 s 9 0482 ‘3 °8596
99647 “ 90620 | 8 "8966

—9 7863 |—1 +9 0753 |—8 "9338
—9 "4781 " 970882 | 89708
+8 0100 ‘ 91008 | 9-0074

+9 '5065 " +9'1130 |—9 ‘0435
9 8005 ‘ “TRAg | 9 °0790
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57 50 20)

71 14 32]
32 32 44
21 18 49
39 53 50)
88 43 12)

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2895] 98 14 34 BH % 42 17} 2908] 95

LUNAR DISTANCES.

2760) 53 27 17/2769] 53 2

3 30) 2648] 24 21 20/2692] 25 49 32) 2619]
19 59}2940] 38 48 31) 2924] 37 16 43! 2909]

2 43)2613] 68 41 Q0\esga} 70 20 23) 2576}
20 94) 2681] 41 57 39)2665) 43 35 8) e6de lh

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352 46 5)2486] 54 27 38} ze92] 56 9 3)m
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93 16 40}3943] OL 45 90 14 12) 2962]

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AUGUST, 1834,

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AUGUST, 1834,

CONFIGURATIONS OF THE SATELLITES OF JUPITER.

At 14", Mean Tue.

‘This Table represents, at 14% afler Afeon Noon of each day of the month, the relative positions of |
Topiter and his Satellites, ax they would appear (disregarding their latitudes) in the focus of w tele
scope that inverts objects, Jupiter in indicated by the white elneles CO) in the centre of the

—tho Satellites by points, ‘The numerals 1, % 3, ord, annesed to the points, serve to .

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AUGUST, 1834.

APPROXIMATE SIDEREAL TIME me
ov Tux
OCCULTATIONS OF JUPITER'S SATELLITES BY JUPITER,
axp ov Tt
‘TRANSITS OF THE SATELLITES AND THEIR SHADOWS
OVER THE DISC OF THE PLANET.

Ooovrrations. ‘Taawsrrs ov Sareunrres.

- AUGUST, 1834,

For correcting the Places of the Fixed Stars,

At Mean Midnight,

Dd

A

449 4217 | +9 9466
11983} 94265 | 99594
10889 | 11861] Q-usi2| 99718

410971 |—1°1796 | +9 4358 |—9 9840
11050 171730 94403 979958
be1i27 | 171661] 974447 | 00074

FL '1201 |—1 1590 | +9 4491 |—070186
11273 11516 | 94533 00296
11342 reta4o | 94375 00403

2O | 411409 |—1°1361 | +9 4616 |—0 0507
at | rl474 | 11279] 974656 | 00609
11537 974696 | 00708

“Ces Ook wee

411598 +9 4734 |—0 0804
14 | 11636 94772 | 0-0898
rajis| 14 94809 | 00990

+1°'1768 |—1" +9 "4846 |—0-1079
17] 11891 94881 | 0-11
11872 9°4917 | 071250

14 12 11-32,

+1192) |—1°0513 |+9 +4951 |—0"1382 }14 8 15 "41
20 | 11969] 10401} 94995 | OvldIz
21 12015 | 170285} 95018] 01489

+1°2059 |—1 0164 | +9 5050 |—0°1565
1eato1 | 10038) 9-sos2 | 071638
been] 09907) 95113} 01709

4-2 2182 |—0°9771 | 4-9 5144 |—0°1778
0-9629 | 95174 01845

12256 | o-g481 | 9-s204| o-1910

—0 9826 |+9 5234 |—0 1973
P2324] 0°9165 | 95263} 0 °2034
12955 | 0-8995 | 9:seo1 | 02093
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WEDNESDAY 10.
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“MEAN TIME.
THE MOON'S RIGHT ASCENSION AND DECLINATION,
Declination. | Df. De [itours,| Right Ascension.

” bom tow “
IN19 33 43°6| 90°27 “4] 124-1
24 12°0| 9660 6 +4] 125-58
14 324] 97°93 126 64
4 44:8] 99-24 “1| 197 68
54 49 °4| 10055 i 128-71
44 461) 101-85 “7 | 329-73
34 34°9| 10314 13073
16 °1} 104 “42 131°72
49 °6] 105 69 ‘ 13270
15 “4] 106-95 i +4| 133-66
33°7| 108-20
44'5] 109-44
47 8] 110-67
43 °8| 11189
32 '4) 113410
13 °9| 114-99
481] 115-43
15 °3| 116 65
35 °4) 117 "81
48 °5| 118 96 c 142-41
54 ‘8] 12009 143-20
542] 121-22
46 ‘9| 122-33,
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38°57 10 12'4

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D First Quarter. .s4.204. stsscoee 9:17 260
© Full Moon. 17 11 18-0
€ Last Quarter... +2515 O64

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192 SEPTEMBER, 1834. -

“MEAN TIME.
LUNAR DISTANCES.

Jupiter
Mas E.

16] 0 Aquile W.

lj} @ Aquile W.
eAnetis EL
Aldeboran EL
Jupiter EL

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Mars

18! e Aquile W.
Fomalhaut W.
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CONFIGURATIONS OF THE SATELLITES OF JUPI’
At i3* 30", Mean Tire.

Rit Apparent West,
+
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‘This Table reprewents, at 13" 20" afler Afeun Noon of each day of the month, the relative pos
of Jupiter and his Satellites, as they would appear (disregarding thelr latitude) im the focus oft
scope that inverts objects. Jupiter is indicated by the white circles (©) in the centre of the }
the Satellites by points. ‘The numerals 1, 2, 3, of 4, annexed to the powits, serve to distin
the Satellites from each other; and their positions are stich nx to indicate the directions of the}
motions, which are in all eases to Le considered ax towards the mumeralr. When a Satell
at its groatest clongation, the pvint ix placed above or below the centre of the nameral, A
cirele (0) at the left or right hand of the page, denotes that the Satelite placed by the side o)
on tho dise of Jupiter, and a black circle (@) that it ix cither behind the dise, or in the wbiadle
Jupiter,

SEPTEMBER, 1834.

PHASES

Mean Time, | Silereal Time, | 14 sean in a Telescope that inverts.

tr a9
wet Seueeba
Seeds

sw
oS

198 SEPTEMBER, 1834,

APPROXIMATE SIDEREAL TIME
oy ome
OCCULTATIONS OF JUPITER'S SATELLITES BY

‘ AND OP THR

TRANSITS OF THE SATELLITES AND THEIR SHADOWS
OVER THE DISC OF THE PLANET,

aa a i

Tagress,

XXII. SEPTEMBER, 1834,

For correcting the Places of the Fixed Stars.
At Mean Midnight,

Logarithms of of the
—} First Point of

D

+9°5347
9°5374
9°5401

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12959
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973603 "2658
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—0 “3562 | 49-5720 “2820 18 10°00
p2sd6 | 95742 “2848 14 14709
01986 | 9°5765 2874 [12 10 18°18

—0 0910 |4-9 75787 |—0 2899
99975 | 975809 | Oo g922
97311 | 9 °5831 “2943

+1271 |—9 2797 |+9 75853 “29638
1/2713 |4+-9°1982 | 9°5875 2982
12712 | 97044 | 975897 "2999

+1 2709 | 4-9°9319 | +9 75918 “3014
12705 | o-osoa] g*5y40 “3088
12700} ov1gus| 95962 “3041

41-2694 | 40-2787 |+9-s983 |—0 3052
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Declination. ; Right Aseension| Declination,
FRIDAY 31,

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V. _ SERORER 1834, 213

MEAN TIME. |
LUNAR DISTANCES.

Venus —-E, | 32 28 21/2346] 30 43 29} 2959] 28 58 55| e973] 27 14 42) 2ay0

0) 2496] 30 56 40) 2403] 32 40 11) 2410] 34 28 S1/2419
‘Venus EJ- - -|--]- - -|--J- - - = ele
@ Aguile E,] 78 56 19|216] 77 22 11} 2900] 75 48 39)2265| 74 15 27) 289%

} Pomalhaut B, [110 55 57 2243/1098 33)2290|107 21 20) 2257/105 34 17) 2266

Sux W. | 42 56 36/2477] 44 38 21/2492] 46 19 45) 2507] 48 0 ag) e522
Fomalhant E, | 96 48 42 e029) 94 7 16,2937] 93 12 10) 9961] 91 27 25) 2367
a Pegasi E, [113 39 36 2602/1121 29/2620 /110 23 18|2640/108 45 17) 2645

|| sox W.| 56 20 $5} 2606] 57 59 222624] 59 37 44]2601] 61 15 43|2660]|
Fomnathaut E, | $2 49 32|245a] $1 7 13)2472] 79 25 20) 2492] 77 43 55) usial
we Pegosi E, [100 37 44/2693] 99 0 56.2704] 97 24 26)2722] 95 48 15) 0736/]

Sux W.]| 69 19 28/2753] 70 54 53/2772] 72 29 58)2792] 74 4 38) 2H10))
Venus W.] 22 49 4/2454] 24 22 22) e060] 25 55 Syl 2869] 27 2H 31)
Pomathout B. | 69 24 0) 2619] 67 45 31/2641 ot

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§ | Sux W.] 81 51 55/2902] 83 24 11) 2920 86 27 33)
Venus W.1 35 9 45/2904] 36 41 8) 2988 39 43
Pomalhaut ©, | 56 31 5/2818] 54 57 0} 2806 51 60 40)
o* iE. | 75 53 10/2995] 74 2 51/3020 jl 343)
Sun W.] 93 59 37/3001] 95 28 59) 3058 98 26 41)
Venus = W. | 47:12 14/3062] 48 41 iy sr 51 38
Antares W.] 42 43° 0/2726] 44 19 6 2738 47 30
Fomathaut . | 44 16 23/2075] a2 47 43/3005) 39 52 5))

| |= Pegusi KE. | 63 45 27)2210] 62 19 30)3242] 60 54 11/a274) 59 29
@Anetis E. [105 21 29/2011 [03 47 ales 102 13 21)eea9|00 39 43)

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Venus W.1 58 55 33/2179] 60 22 14)3157] 61 48 3yjai99] 63 14 SO)
Antares W.]55 24 4/2824] 56 58 1/2836 60 3 yg
a Arictis, E, | 92 55 43/2916] 91 23 44|2928] 89 52 0/2941] 88 20 33)

1| Sow W. [117 13 4)3266]118 37 55)3277]120 2 Sal azes}121 26 5:
Venus W.} 70 22 16,3266] 71 47 7)3277| 73 11 adjaes7] 74 36 1:
Antares W.] 67 48 55/2909] 69 21 2) 2920] 70 52 56) 2929) x a

| |wArietis EF. [80 47 1/3011] 79 17 2) a02a] 77 47 17) 9034 Wy 1

E, [111 23 40 2901]109 51 2z!2909/108 19 15) 2920) hie 47 21) 2929]
Supiter —E. [t15 51 26/2e70]114 18 $4)20e0}112 45 S3)e¥9a 111 13 24/2901)
Venus W.] 81.35 46jaa39] 82 59 12/2347] 84 22 29)s954] 85 45 38) 3362
Antares W.] 80 0 28 2078] 81 31 S/2985] 8S 1 39)2993] SH 32 1] 2999]
mArietin E. | 68 53 31/3098] 67 25 20|a109] 65 57 21/3119] 64 29 33] a120]

E, | 99 10 38/2970] 97 39 47/2978] 96 9 6j2985] 94 38 3h 99]
Jupiter E. [103 33 44/2942]102 2 18/2950]100 31 2|2987] 98 59 55) 2968)
Venus = W.

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Antares 92_1 sBlacz9] 93 31 29)a008| 95 0 59,3039] 96 30 23] soxa}

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LUNAR DISTANCES.
P.L, PL, BL, Pet
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on oon ore

‘32 28 2)) e346] 30 43 29/2959] 28 58 55/2373)
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96 42 42 0523] 94 57 16) 2337 93 12 1O\ess1] OL !
113 39 86 2602}t12 1 25) 2698 ]110 23 18)

56 20 33) 2606] 57 Sg 22) 2624) 59 37 44/2640
82 49 32}2483] $1 7 13)2472| 79 25 20) 2492
00 37 44)26941 99 0 56/2708] 97 24 26)2729)

69 19 23}2753] 70 54 53)2772| 72 29 98/2791
2249 4}2ass| 24 22 go]2n60| 25 55 32] 2869
69 24 Ojasi9 te 45 32)2041| 66 7 32) 2606) 64
87 52 84) ese9] 86 18 36/2840) 84 45 3) 2060)

81 SI 55|2902] 83 24 11) 2920
35 9 45/2044] 36 41 8}2958
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75 33 10/2995] 74 2 SI} s020

93 59 37}3041] 95 28 59/3058
47 12 14] 4062] 48 41 10) 3077
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CONFIGURATIONS OF THE SATELLITES OF JUPITER.

At 13", Mean Time.

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‘This Table represents, at 13% after Acan Noon of each day of the month, the relative positions of ||
Jupiter and his Satellites, ax they would appear (disregarding their latitudes) in the focus of a tele- jf
scope that inverts objects. Jupiter is indicated by the white eircles (0) in the centre of the page ; |
—the Satellites by points. The numerals 1, 2, 3, or 4, annexed to the points, serve to distinguish
the Satellites from each other ; and their positions are such as to indicate the directions of the Satel-
lites motions, which are in all caves to be considered ax fowards the numerals, When a Satellite is |
at its greatest elongation, the point is placed above or below the centre of the numeral, A white ff
cirele (©) at the left or right hand of the page, denotes that the Satellite placed by the side of it is
on the dise of Jupiter, and a black circle (@) that it ia either behind the dise, or in the shadow, of |
Jupiter.

Days of the| yy,
Mouth. tae,

PHASES
as seen in a Telescope that inverts,

85

BoGkSa

APPROXIMATE SIDEREAL TIME
ov rane |
OCCULTATIONS OF JUPITER'S SATELLITES BY JUPITER,
‘ano ov 7HE
TRANSITS OF THE SATELLITES AND THEIR SHADOWS
OVER THE DISC OF THE PLANET,

Oceusrartoxs, ‘Twawsirs ov Savennrres.

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Sun. |
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44 15°10
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16 27 3722
16 31 33°78
16 35 30°34

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B, | 38 11 52 sors] 50 41 55) 4009] 29 13
Haiecan 34 34 Se) ai03] $3 6 48] s102 ar ap ar] hua 30 10 34/s109
‘| Mars E. | 76 37 $8)a96s) 78 7 Ba964} 73 86 4) ngs9] 72 5. Ojos
Pollux BE 39 27|2063) 77 10 99) 3064) 75 Al a8) 9060] 74 12 46)0006
B) a Aquilm W.|104 43 38}ae39]105 58 6) 494]107 12 15] sen9]108 26 B3}a867
Fomalhaut W. BR 205 1s 76 10 98\ 9180) 77 36.57] 297°
Jupiter BE 9 39) 2979 n) 17 7 SBlagb1p = = + [- -
Mars | 64 27 54) 294] 62 56 Gist GI G4 10] 2910] 59 5B A)zs08
Pollux | 66 46 23) 1029] 65 16 46) 3028] 68 47 2] s01:
| Fomolhout W.| 84 $1 $6 19 S| sie7] 8) aging)
“Ja Pegasi W.| 67 43 $9 4 Adj aioe 5 oe Blas
t Mars E.]s2 9 50 36 14)4997] 49 3 0} 2849]
Pollux = -E, | 54 45 53-15 §)2969] 51 44 13) 2982]
| Regulus B. | 90 48 89 17 27/2968] 87 46 $4] 4960
44) Fomothauw. | 96 35 98 4 S0}a064)
I ene W.| 78 42 80 6 Sans
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| F. | 42 35 Al 3 S0/api0
| | Regulus E, | 78 37 77 «5 34/2902] 75 33 18} e093] 74 0 50) 2885
S| Fomlhaut W. [108 29 43) 109 59 33) 3015]111 29 27] so1of 12 59 27] 9006
pies W.] 89 57 53] s2a2] 91 23 16)a238) oa mw] 4 14 Bd) 219
o tin «WW. ] 46 39 49} s056] 48 8 53| 9095] 49 38 Bel s017] 52 SB 1d) e099
Mars E. | 86 58 1ojaye6] 25 22 dje717] 23 45 dG} ares] 22 17) 8699
| | Pollux — E.| 80 16 etl OF $8 Siraeel ar oo gyeeee 29 Si) ees
Regulus E.] 66 15 49) 2002] G4 42 16javsa] 63 8 Se] esos] GI 34 37)e07
| [Saturn EE. [119 56 Glevse]11¢ 22 54]2847/116 49 27] daae]ti5 15 49] eeae
16 Pe W.] 58 42 52}2920] 60 14 46}2906] 61 46 57] 2293 5.9 5 2079
| nee W.} 29 36 31) 2715] 31 12 51}2706] 32 49 23} 268] 34 Gj 2690
W.| 27 13 1)]2017] 28 47 17}2808] 30 21 41]47h9] 31 56 St)e776
| [Regulus E, | 53 42 19} 2776] 52 7 19}9769] 50 32 10/4760] 48 56 Sul e760
| [Saturn —-B, [107 24 SF} 793/105 49 47]2775/104 14 46)a766]102 99 $3) 2757
| [Spica me E, [107 44 25) 2705/1069 87) 2776 ]104 34 86) 2746]103.89: 24) 2757
T]]eArctis W, 72 39 49}000] 74 14 5} a709] 75 48 34}t780
ya sl 44 10 25/9633] 45 48 26) 4630] 17 26
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| [Regulus EL 39 2 31/9701] $7 45 Gl aza7] 36) & B5)2701
) | Satan: E G3 4 12)2705] 91 27 38] 2696] 49 50,53) 2687
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18] @ Avietis W 85 19 S9la7sa] 86 55 Ss]a7ea] 88 BZ 3) 2716
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16 20 | 0-86 | 8-93 || 0-45 | 1595 |
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26 | 0°99 | 10-20 0-42 | 1 28 | 0-81 | 8°39 | o-44 | 1-49
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MEAN RIGHT ASCENSIONS OF 100 PRINCIPAL FIXED
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13:16 red ‘a

29607)
13 51 54°53 + a-t972|-+-0-0414;
14 754-64) 2-enis|

1428 ga 474723)
44-37 33°77| 2-600

15 27 29°59

@ SERPENTIS - 15 35 54°05 |4 2"9281/
jhe 15 50 18°69 |— 23964)
iy i 15 55 33

8 Ormivenr = 16 5 26°69

@ Sconpir ~ ~ 16 18 59°76
66| y Draconi 16 21 42-11

Le ele awe

2
Ss

ECLINATIONS OF 100 PRINCIPAL FIXED STARS,
FOR JANUARY 1, 1830,

+15 31 20-7]
+54 38 20

ue} scape 1 Hh *9 23

-3|—22 27 16

$39 14 184
1 |-10 16 147
+50 9 527)
+19 15 12°7)

|—59 32 55 -1]—17 7127]

a7 ma
7 3475) 16-009:
+27 47 43 ‘ 16 "5008
I-15 19 45 -5\—19 -2802}
474 51 14) 14-710

— 8 44 58°5) 19 636:
+27 17 31-4) 12-300

+658 0811-796
$78 18 4778] 10-752:
—19 19 554] 20"3628)
is 3 14 57°56] 96129)

26 2 436 e355:
+61 54 2-4) 8-981)
—68 42 6'2) 7-6149)
—89 14 58°6) 5 5H24)

2 anem uvwe!

482 18 11°6)\— 48796)
+14 35 27°38} 4-6055)
+52 25 49°7} 29129)
$12 41 27 °3] 278739

ao
*

ry
& net ee

Bu
Se

Seow w

o
cS

a
3
8
3
2.3

3
2
3
1

‘The numbers in the columns ¢,
the following formulw, viz.

of salt

* wt a
foatipe T+ Ersas

Se ee

MEAN DECLINATIONS OF 100 PRINCIPAL FIXED STARS,
FOR JANUARY 1, 1830,

w
(i)
. ta
(4 ~$une(43)— w X42 =y} ua"
peti fs 1830,
I = 460529316; m” = 0'000308645
vies nay = DO'OS0G5S4; w= 0" copegyeent Bussnu's Tab. Reg: p. x,
@=cose tin’; b= sec*d i"; rss tan @ sin 1",
@eatnds | Pabines potas aniy Rasta tond

sau (St)40($P
rae Sedov Bonde) (HP

‘The annual proper motions, Ac and Ac’, are thove adopted by Mr. Barney,
dn the Astronomical Society's Catalogue, except for a and 3 Ursm Minoris, which
JP] have been taken from Brssea’s Tad. Reg. at pp. xliii and sly,

2288 S888 £58

gee sees

A
&

SHSS Seah SEGa os2BS Sess
wee awe

Bose 8

31078

N

31254 | N.

2
sciebe
an4061

“2°8782

1932)
ae Mh eae
28556
373926

+ 3°8577

8.1
Nw
NA
5.

ZZZ" www
& shef «tae

SB

Pur BaaA Bwoy
SESE inees
Stex Soesrases

we*

MEAN PLACES OF 100 PRINCIPAL FIXED STARS,
FOR JANUARY 1, 1834,

Ze

4
A 45 ares + ae pak
2 8 47°33 5
1217 i! “306 Bert soe
12 25 40917 3'1$22 |S. 22
12 48 15°290|4 28422 |N39
1316 27-458 31498 |S.10
13 40 59°376 2 °35379)N.50
13 46 47 218607 |N.19

18 52 11085 S.59 34 5°93
IN:

1°53

15 27 39-700

15 86 5 '803
15 50 9161

15 55 47 annie
16 5 39 °238)

16 19 14 1406/4
16 21 45-283
16 31 10°110
17 2 97135

17 8 14-290
4°906

N.S1 30 40°85
S.2t 5 35°60

18 43 57-209 |4

18 57 46-9; 27565 \N.13 37 23-18 | 5-005
19:17 7-25) 30087 |N. 2.47 25-16 | 6-625
19 38 22°105/4 2-asi2 [N10 12 52°76 [4+ 8348

a
EE

z
i

a4

MEAN PLAOES OF 100 PRINCIPAL FIXED STARS,
FOR JANUARY 1, 1884,

Ae al
‘Names of Stars, Right Ascension. | Anmusl Var,

+ ms +
@ Aquinz - 2/19 42 41 -062|4+ 2 -92559\N.
B Aquinas - 19 47 9°620) 2°9448
a*CaPRIcoRNt 20 8 50°351| 38-3325
90 12 27 -882/4 4°8116

20 26 31 °096|—48 6973
20 35 46°546|4 20415
20 59 28°171| 2 °69034)
21 5 52°542| 98-5462 [NS 14548

a@ CEPHEr - - 21 14 36°659 14171 [NJ +15 057
& Aquantr - 21 22 48-925} 3 "1637
ACrrngr - 21 26 29 °363} 0 °8099
« Pegasi- - 2186 2°077| 2°9442

@ Aquarit- 21°57 15-425 30836
@Gruis - 81 57 43660} 38189
£ Pegasi- - 22 33 11°104/ 29835
@ Piscis, Aust. 22 48 27 °560 3°3120

a Precast 22 56-29 887|+ 2 °9769 |N.! 31°36
+ Pisciu «5/23 31 24-916 30565 |N. 89°10
Cephei. 23 32 36°066| 2 °3957 22°35
a@ ANDROMEDA 23 59 49°317/4+ 30698 |N.28 10 26°73

‘The Mean Places and Annual Variations of the 100 Stars for Jan. 1, 1834,
contained in the preceding Catalogue, have been deduced from the Cotalogue for
1830, by means of the following Formule :

Let o/ and ® represent respectively the Mean R.A. and Declination, and A «,
AY, the Annual Variations, of a Star for any Epoch (18304). Then,

dat (othe) th ety ie

Yose(pacyte Pong Lye
SPt + dey et iO + i95 !

adaotact F tei) + (sttesery)

,
A¥adtad4 PF ete 4% Orssten

The Annual Variations, into which Ac and Ac’ enter, are distinguished by
an Asterisk,

FIXED STARS.

FORMULE OF REDUCTION,

ACCORDING TO PROFESSOR BESSEL.

1.—Adopting the Notation and Coeficiente employed by Mr. Baily, in his Intro-
duction to the New Tables of the Astronomical Society of London.
A= —18°6768 cos ©
B = — 20'3600 sin ©
C =t— 0°02495 sin 2 © — 0'34362 sin 2 + 0°00413 sin 2 2 — 0°004 sin 2 €
D=-— "5447 cos 20 —9'2500 cos B +0'0903 cos 22 —0°090 cos 2 (¢
@ = cos « sec 3
b= sin a secd
c= 460206 + 20'0426 sin @ tand
d= cosa tand
a = tan w cos 2 — sin sin 3
Y= cose sind
¢ = 20°0486 cos a
@=—sing
‘Ac the annual proper motion in Right Ascension,
‘Ad'= the annual proper motion in Declingtion,

‘Where ¢ denotes the time from the beginning of the year, expressed in fractional
parts of » year, © the Sun's and the Moon’s true longitude, 8 the mean lon-
gitude of the Moon's node, and w the obliquity of the Ecliptic, each for the time ¢:
athe mean Right Ascension and 2 the mean Declination for the beginning of
the year. ‘Then for the time represented by ¢,

Apparent R.A. =a+Aa+Bb +Cc +Dd +tdc.
Apparent Dec, =3 4+ Aa! + BY + Cec! + Dd’ + tdc.

%.—Uring the same Notation and Cogfficients, and assuming

46-0206 C=f Boh cos H
20°0426 C=¢ cosG A=h sin H
D=g sinG Aten wi
Apparent R.A. =a + f+ tac

+ sin (G +a) tan 344 sin (H +a) secd
Apparent Dec. = 3 + i cos 3 + ¢Ac’

+ g cos (G+ a) +h cos (H+) sind

372 FIXED STARS.

+2184

$3117

352 40
352 35

+2032
20°35
20°36
20°34

+20 ‘30

seus

374 FIXED STARS, '1834,

- wee

con ae

8 885 eee

35

oe
3391
56-00
3610
36°21
36°32
3643
86°56
36°70
86°83
36°97

$g2 S8e se¢

‘8

APPARENT PLACES or « axe 2 URSA MINORIS,
FOR THE UPPER TRANSIT AT GRERNWICH.

a. |
2 8,|

3s S25 2

r=

SS

53
oa
58
52
ot
ot
50
50
56
4g
a9

S82 S88 288

eu \
92

SRR SRF SOL SSS SEF F:

ede" G22 sag e83 £.

FIXED STARS, 1834. 375

2 URS MINOR. B= 4 URRE MINOR,
RA | Dee W. [Mow Roae | Deo Ne
bowl oy k=l oo 7
86 34 0 59 | 88.25

. D

=
eae

Bes

$2 Sho 258

376 FIXED STARS, 1834.

APPARENT PLACES or « ano 2 URSE MINORIS,
FOR THE UPPER TRANSIT AT GRERNWICHL

RAL

=
@arss starr OAD aun. DL
eye

Zee 682 388 ead v

HSh £8S Sau

APPARENT PLACES oF « axp 3 URSH MINORIS,
FOR THE UPPER TRANSIT AT GREENWICH.

Cen see

S88e S8& SES

378 FIXED STARS, 1834.

APPAHENT PLACES of « ssn 2 URSE MINORIS,
FOR THE UPPER TRANSIT AT GREENWICH

SEE ES

2
36
oe
27
“Ot
00
37
3

S85

FIXED STARS, 1834. 379

y APPARENT PLACES oy ¢ axv 3 URS MINORIS,
FOR THE UPPER TRANSIT AT GREENWICH,
NOvRIBER

2 URSA MINOR.

Day
ined
, | Month. ;
86
”

RA. | Dee. Ne
© =lae a
1 0 | 88 25

S eeu ove Gun

APPARENT PLACES OF THE PRINCIPAL PIXED

3-5-4

S28 S88e
eecun =

3
288 see

s

6
6
6
6
5
5
5
5
5
5
5
5
5
6
6
7
7
7

NPPARENT PLACES OF THE PRINCIPAL FIXED STARS,
FOR THE UPPER TRANSIT AT GREENWICH.

e wusep B

Peet at

édas agd2 2¢
#2232223 ues 53

dive

Sf S8SE E825 BER S

S.3 #8¢ 3

3s
A

FIXED STARS, 1834;

Srm-8

a
ul
a
a

sess

ee Sy ee
SS SaS5 880 8Ee8 Se8S

z

384 FIXED STARS, 1834, 7

APPARENT PLACES OF THE PRINCIPAL FIXED STARS,
FOR THK UPPER TRANSIT AT GREENWICH.

eeue

geese =<
SSSe

g$8 GSss S8se

82
. "
3410 * [62-21
ae es
‘03°
33°94 °' 165-93
ow
33°81, .,,|66-74
3 65 $167 30
48 °"7)67 G1

33
9) 33-30 ° 1167-06

37°01 |. 13368
3702 15519

‘APPARENT PLACES OF THE PRINCIPAL FIXED STARS,
POR THE UPPER TRANSIT AT GREENWICH.

= "6s BESTE

28 S885 485. "5-8 Bes S85

=
Bo

SS SaSS sbSe2 ESe8

FIXED STARS, 1834. 387

APPARENT) PLACES OF THE PRINCIPAL FIXED STARS,
FOR THE UPPER TRANSIT AT GREENWICH.

[reson [tn G_|
ia CE
e

+ @e it tts

or ae

a
1
a
31
oO
20

2
is
Pra

1
n
a

my
ity
a
aL
10 |
20)
30
to

on co oo

[> RO
SS uBEe Bes SoSE

o}t09 “21
so-ar ° hi14 -05

-

-
i

22

1
u
a

1
u
a
aL
to
20
30

£

ae

eore cous,

<
é
a

362
36 a 2)

af

aeee 56

1400,
qe 61 *

* sued
Sa Sanam
oe Se}

aed

9

.
25
26
26°
26
26
26
26
26
96°
26°
26°)

ré
23 ,,,|9015
+54 979) 53 61 2%

ob 37 2
oben °™ 56 26

49 "23
48 47

sete: Be

-*
|
h
une |

uu
2
a
10
20
80
)
20
30

]
Ay
ag

—ig>

2 oF

a
BS 8.85 Sbhe Bee

as

teen

eng oe

Bt See

1

*
3
4
4
4
5
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5

$e

a oe Se eee

°
8760 AL'S
37) s795 °|39-45 8

$8 828 seas S336 gies Seas s8e2 Sen

Ue Buys 2yse S2ee e825 SF2F =

é egeg 8-
sé

&
Sees SS

e@oc © ees © coe,
&

re
aius $6

at

=
3
8
4
“46
40)
2
“26
ni
ua
08)
03)
“09
ons
oup

& S25f S4e8 SERS

Seos8 5385 S85~

goa case o

26
26
26
27
27
27
37
28
23
28
2s
28

S S555 8555,
ase vues Ssee

Ey
ty

£ SSSR SSSR KF:
gu gdee Sega 28

FIXED STARS, 1834. 397

APPARENT PLACES OF THE PRINCIPAL FIXED STARS,
POR THE UPPER TRANSIT AT GREENWICH.

ona
te ous feed ony

198
99 4.
“85
a7
61

ae

43
43
“3
43
“3
43
43
a3
43
43
43

25.38

we
FIXED STARS, 1834, 899

APPARENT PLACES OF THE PRINCIPAL FIXED STARS,
ror

mi
fe
F
ss
lent.

al
2
a
30
10
20)
30
9)
9
=|
8
18)
28
ct 8}
18
28)
w
Wy
27
£7
a
ash
37

APPARENT PLACES OF THE PRINCIPAL FIXED
FOR THE UPPER TRANSIT AT GREENWICH.

foo OF
see

22.2 338
22 S822,

eee $494.
See ssa 7

=5
oe
SS

4

FIXED STARS, 1834. 401

APPARENT PLACES OF THE PRINCIPAL FIXED STARS,
| FOR THE UPPER TRANSIT AT GREENWICKL

ABAD 6 gf 12252
43-73 °*) 9-06 94

SEoe,

tates Bare sees
S828 uate Send wes dees

S328

Sewe

o
°
o
°
1
1
1
2
2
2
2
3
3
3
3
5
4
4
4
8
3
3
3
3
3
2
2
2
2
1
1
1

Sees =

S8e8
Siu desu 8

BINED STARS, 1844

APPARENT PLACES OF THE PRINCIPAL FIXED STARS,
YOR THE UPPER TRANSIT AT GREENWICH,

they
S45 97/61 3g *

2E=

SoSS

SG osSee Bek

SS

* o
44 3605
weed On| so aq7 28H

APPARENT PLACES OF THE PRINCIPAL FIXED STARS,
‘FOR THE UPPER TRANSIT AT GREENWICH.

SRRE fess.
$628 8224

4 O08 ..
a3 Tot

162
168

APPARENT PLACES OF THE PRINCIPAL PIXED
FOR THE UPPER TRANSIT AT GREENWICH.

12 29°99 1, 19 36"90
23°96 °°? | 34-83

ro Fe Gk
$8 Su8S s8ee Bead cess

=
2s
25
"25
2
25
23
25
26
26
26
26
26
26
26
27
27
27
27
7
27
a7
27
7
26
26
6
26
26
bad
2
23
23
25
1
Ey

=

8h S¢éu S86 ve

aes suse as

88 oS8S 8455 Be4u BOSR BSS wESS SErw Bake seas
a wda2

7]

PLACES OF THE PRINCIPAL FIXED STARS,
FOR THE UPYBR TRANSIT AT GREKNWICH.

aSsn

Sa35

25

& Aqrvanit.

RA

3°09 9, 7361
305 °° 74-33 1 28

FIXED STARS, 1834.

" APPARENT PLACES OF THE PRINCIPAL FIXED STARS,
FOR THE UPPER TRANSIT AT GREENWICH,

a
2

*

45°10 38 53
45-01 2 37°29 ite

ons
$2 enlist
30°29 9°99) 46-34
30°27 °/4g-a5 14

(PTE
RE
ES

+ 0'-0206 cos weed |
aad for tho Lower Transit, |
00206 coe p sue 2

TABLE,
Showing the Correction to be lied to the preceding
me Poke Bam Bor Ua orem of Rees eb

ese

eveesees

é

ww
02
“or
“08
+09
“03
03
+09
“04
+04
“06
“08
“03
0
“03
“es
+06
sos
ses
<6
or]
Sacl
“97
a
a

Ssseseseget

aitss

TABLE,
wing the Correction to be upplied to the Apparent Places of Five Polar Stars, _
for the terms of Nutation involving 2,

e222"

age

-t- 109 | 1012 | 209 [+ 168 Bor

Sore —When tho Argument in on the right-hanil side of the Tuble, the signé of the
‘correetions must be changed.

aa

Ty TE

‘Libra:
Libre
‘Liber

FE TT
RAY eR

16 19 12-10

16 19 12°13
16 3432-14
17 3 10-05

if

F
“<i =|H=

7+

17 82 418.
is 1 774

18 30 1235
18.59 8°65

19 25 30°04

19 53 43°39
20 21 24°81

BE fa -Be

20 43 27-69
21 M4 49713

PHPGP ETP GRE

£ th be

ee
Sae3

Ske Seas
ween

Seen

22
22
bid
23
ee
23
23
23
23
3
o
o
o
o
o
t
t

Sf8e «SSS

oe
sa se

BSneo eeltoe ease eee mwas

Evan of

Sere

Safe,
ts eee

Bees
Bebe SS

Ecesk Susees

aunt
riggers
oe oe
Bsskss es
SEG8 SBR.58 Teesss Gresss SSREn Bssess Gees

4
e

Beaks Sstesa
wate

pa Orn
Bean w
ee ae
SExSSR &
a
®
C2

eae ow
BSS

10 56 27°37
10 49 31°90

= «e=S58a

Wap

ayes este

1142 3°21

11 87 19°74
11 42 3°23
11 42 37
18 10 $2"

So

S2 Besse SElSe =.

12 98 1905
12 33 15 08

13:16 87715
13 26 1425
13 33 1140
M40 L4"i7
Mal aye

V4 41 4177
V4 97 17 32
14 54 86-65
15 26 14°05

15 06 14°09

16 2 povse
16 19 1296

16 2 g0°35
16 19 13°00
16 17 1549
16 45 R435
Pp Ophiuchi- - - WL 188

p Ophiuchi- - -
fon IT. Les
Moon IJ, vu.
pw Sagittari - -
p'Sngittarii -
Moon II.
Moon I.

Moon ll. 20) & 0-03
Moon Tf. v. 36 748

Moon LU. ¢. 8 49 80
Moon Il. uv. SL 135

Moon II, S7 37°73

Moon II. vc) (29'S) 23 96°53
Moot. hel - - 46 48°28

ULMINATING STARS.

At Greenwich Transit.

Moon I.
Moon I,

Moon I. 22 59 1912 | 116-89 JS.11 28 | 6211

MoonI. Le, 23 22 .28°78| 11480] 9 16 | G19
WAquarii - 2310 17°64) - - |S.10 31 | - -
Moon I. 23:45 1601 | 11316 6 58 | 61"
Moon I. 0 7 46°47 | 112-01 436 | 604
+ Piscium 2353 95°22| - - |S. 656 | --

7 Piscium . 23s3es21| - - |S. 656 | -
Moon f, v.c| (3°9) | 0 30 6°31 | 111°39 |S. 2 12 | 607
Moonl, .c| - - | 0 52 21°98 | 111°32 |N. 0 14 | 607)

¢ Piscium 059 48°25| - - |N, 446 | --

e Piscium o5sg 4824) - - 446 |--
Moon L. 114 40-22] 111-82] 2 39 | boy
Moon I. 137 soz | 112-91 5 4/62

» Piscium - - 1 32 46-82] - 439 as

© Piscium 136 36'37| - - |N. 819 +

132 4631| - - IN. 439 | -
1 36 36°86 819 >

1 59 52°53 | 11461 7% | 617!
223 1700 6-91 g 45 | 6241
219 19°54 743 | --
227 930| - - IN 452 | - -
219 19%3| - - IN. 743 | - -
227 929) - - 4 52 :
246 40°74 | 119-81] 11 59 | 63%
3:10 58°84 | 123°30 | I4 7 | Oe
318 l0e2| - - IN.9 9] --
3181020| - - |N.9 9 | -
3.36 2°08 127733 16 7 ie
4 1562/1312] 17 58 | 6631
351 28-91) - - 181-1: |} 2.5
41020770) - - [N15 13 2
35198%9/ - - INIZ 1] --
410 20°68 | - - 1s 13 | --
428 47-09 | 136°66| 19 36 | 67%
456 141-68] 21 1 | ow
4 ‘We ast
5

MOON-CULMINATING STARS. 421

v.c} (101) 25

hel - 9+ 55

* 5 a

| 4
49 cr

4

25

= oe
sea

Swe saan Oooe

20 a4
10

29

; 1

@ Geminorum 43

pi Concri- ~~ - 56

Sau aw
oe

2 743
7 56
13-2)] 8 34
ohh 9 6
5.6 | 8 59
45 19
22 i --| 5.6 8
i --| 45 | 9
Moon T. v.c) (14°3)] 9
MoonT. hel - - | 10
-s 9
i * 10

23

14937
1143 1st | M712] 723
Wwiussll| - - IN

wc) (16 3)
¢ Virgins - - +| 5.6

ce Virginis ~- | 5.6

2 Wisse) - -

4
N. 4 4
12 12 12-20 | 144-74 | 4 18
rit

4

Moon ti, le) - =
Moon IT, v.c] (17 '4)| 12 40 57°13 | 14284 N.
© Virginis - -+| 4.5 | 13 122°30| - - |S 489
13 16 27°33 | - - |S.10 18

« Virginis + - = 1

15

16

Mag:
nitude,

wen ee

MOON-CULMINATING STARS, 423

120°31
117 "80

115-65

11397
52 28-21 | 112-62

174
Mist

Tita
112-06

44 19-35 | 113-21
7 7758 | 1488

19 19°20] + -
30 1882 | 117 08
53 59°57 | 119°79
50 47°88 | +

50 47°87
18 15°74 | 182-99
43 12 ge | 196-61
$1 B86

51 2845
8 55°87
35 28-29
26 23-29
53 101g

arr

... LMINATING STARS!

+ Leonia -
2 Veanin-
Moon TI.
Aloon I.
p Leouis -
3 Leonis -

29 |p Leonis-
3 Leonis -
Moon I.

Moon I.

» Virginis

B Virginis

Moon I.
Moon UL.

15 26 15 67
15 94 4543

17 49 38°77

17 33 28 86
17 49 38 ‘80
17 32 061
18 1 40°38
18 35 16°68
18 44 57°73

18 35 16°72
18 44 57°76
18 31 5 68
19 0 8°37
19 26 $531

19 26 3534
19 28 42°31
19 56 41 24
20

20
20
20
20

17 9°57
27 45°39

Be
GuaSs TEl8o BeBS

ae a
BEBES Hasse sess Sse

me
Hare t Se

e
8s §
ga ¥.

al 16'37-07
21 an S311
21 57 8671
21 57 26

PoeR
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MOON-CULMINATING STARS. 453

OCCULTATIONS OF FIXED STARS BY THE MOON,
VISIBLE AT GREENWICH.

Magnitude.

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‘The Angles are to be reckoned from the northernmost point, und from the vertex
towards the right hand, round the circumference of the Moon's image, as seen in a
‘Telescope that inverts,

‘The Apparent Places of the Stars, on the days of occultation, are included in
the following Table.

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‘The preceding Table contains,

1.—The Apparent Places, at Greenwich Mean Midnight, of the fixed Stars to the
6th magnitude inclusive, the Occultations of which will be visible at Green-
wich.
2—The Apparent Places of all Stars to the 5th magnitude inclusive, the Oceul-
tations of which will be visible at some part of the Earth.

3.—The Greenwich Mean Time at which the Moon, to an observer at the ceatre
of the Earth, would appear to have the same Right Ascension as the Star.

4.—The Difference of Declination and Position of the Moon, as it would appeer
with respect to the Star, at the instant of Conjunction in Right Ascension

5.—The Parallels of Latitude beyond which the Star cannot be occulted by the
Moon.—Between the limits here given there will certainly be an Occultation:
but whether it be visible or not at any given place must be determined br
other considerations.

PHENOMENA, 1834.

ECLIPSES OF THE SUN AND MOON.

Is the Year 1934, there will be three Eclipses of the Sun, and two of the Moon.
‘The only Eclipse visible at Greenwich will be that of the Moon, on Dec. 15.

I—A partial Eclipse of the SUN, Jan. 9, 1834, invisible at Greenwich,

Begins on the Earth generally at 9* 16% Mean Time at Greenwich.
Longitude 100° 31’ FE. of Greenwich. Latitude 52° 43’ S.

Greatest Eclipse (5°3 digits) 10% 55™7,
Longitude 11° 7! E.of Greenwich. Latitude 67° 47’ 8.

Ends on the Earth generally at 128 34™6,
Tgngitude 69° 25’ W. of Greenwich. Latitude 48° 33’ 8.

This Eclipse is visible only in the Southern part of the Pacific Ocean, and the
Southern extremity of South America,

IL—A partial Ectipse of the SUN, June 6—7, 1834, invisible at Greenwich.

Begins on the Earth generally June 6* 19" 57%0 Mean Time at Greenwich,

Longitude 2° 41’ W. of Greenwich. Latitude 47° 44’ 8.
Greatest Eclipse (11°2 digits) June 6" 22° 8",

Longitude 54° 53’ E. of Greenwich, jatitude 64° 30” S.
Ends on the Earth generally June 7* 0” 20™0,

Longitude 72° 19’ E. of Greenwich. Latitude 27° 32’ 8,

Visible in the Southern part of Africa ond the adjacent Sens,
At the Cape af Good Hope, the Eclipse
is Baik kaes
eee a ona { Mean Time at the Cape.

Digits eclipsed 5°4 on the Southern limb.

IIL—A total Eclipse of the MOON, June 20, 1834, invisible at Greenwich,

First contoct with Penumbra, at - - 17 31°)
First contact with dark Shadow, - - 18 32°3
First total Immersion in dark Shadow, 19 36:6
Middle of Eclipse, - - - - - - - - 20 19°3) Mean Time at Greenwich, |

Last total Immersion in dark Shadow, 21 24
Last contact with dark Shadow,- - - 22 6°7)
‘Last contact with Penumbra,- - - - 23° 7°
Digits eclipsed 16°7 on the Northern limb.

IV.—A total Eclipse of the SUN, Nov. $0, 1884, invisible at Gy

Begins on the Earth generally at 4° 41™9
Longitude 141° 9 W. of Greenwich,

‘Total Eclipse begins generally at 6* 0™7.
‘Longitude 133? 50’ W. of Greenwich.

Total Eclipse at Noon - - 6" 33™0,

7 | Longitude 101° 3’ W, of Greenwich,
‘Total Eclipse ends generally - 7° 523.
Longitude 49° 39° W, of Greenwich,

Ends on the Earth generally - g* 11™1.
Longitude 57° 267 W. of Greenwich.

‘Tho Southern limit of this Eclipse, or the line traversed by the
of the Penumbra, passes over the places,

Longitude 154 35
1g 14
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80 33
50 30
42 e3

‘The centre of the Shadow, or the axis of its cone, passes over the

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Longitude 183 50
118 10
109 36
104d 4
99 34
95 31
91 39
87 43
83 31
78 46
231
63 57
49 99

REPRESENTATION OF THE PRINCIPAL LINES FOR THE
SOLAR ECLIPSE OF 34.

‘The first contact of the Moon's Penumbra with the Earth takes place at B,
‘and the partial Eclipse then first commences,

‘The first contact of the Moon's Umbra with the Earth takes place at C, and
the central and Colat Eclipse first begins.

The Moon's Umbra passes over the places situate on and near to the line CC’,
causing at ench in succession a tofal Eclipse. The last contact of the Umbra with
the Earth takes place at C’, where the total Eclipse ends.

‘Tho southernmost point of the Penumbra comes on the Earth at L, and pro-
ceeds along the line LL’, quitting the Earth at L’, To all places situate on the
line LL’, the limbs of the Sun and Moon will appear in contact. South of this
line no Eclipse takes place, The Penumbra quits the Earth at E, where the par
tial Eclipse finally ends.

On the line LBP, the Eclipse begins at the instant the Sun rises, On PSL’,
it begins when the Sun sets. On LRP, it ends at Sun rise, On PEL, it ends
ot Sun set. The places on LCP have the middle of the Eclipse at Sun rise, and
on PC’L! the middie of the Eclipse ut Sun set. £

+A partial Eclipse of the MOON, Deo. 15, 1834, visible

Fit contact with Penumbra, at 11 0"3
First contact with dark Shadow, 15
Middle of Eclipse, 16 47-8 } Mean Time at
Last contact with dark Shadow, 18 16-8 rt
‘Last contact with Penumbra, - 19 3573
Digits eclipsed 8 “1 om the Southern Timb.

[At these times spectively the Moon will be in the zenith ef the

Greenwich Mean Time of Ecliptic 8

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Sind

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¥ in Aphelion,
3d oSagit, *
hé@ --- kh
OR as) — 0

FEBRUARY.

BeOS
A OARAA

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np. 8 ©
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Capricor, * 1 24S,

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? greatest Hel. Lat, 8, !
oeoq --- $2 5N,

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Ud@ --- H3S20N.]
Qdqd --- 9 343N,

& greatest elong. 18 22 F,

dq --- ¥742N.

“dq -+- 43 28N.

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1615 22 ¥ in Sup.dO

191417 Sind

23 1 7 enters, Autumn comm’ udC --- HO 2S
312 - dd uGemin. € 0568.1191747 GeO

Wa239 dC --- %O 48./ 201458 SdC --- SOseS,
2412 0 in Aphelion. 2017 20 Fink

18 2 gé¢ --- $1 0S.

272110 ¥déh --- $i sas. Stationary.

21742 g00 § in Perihelion. !
$0 9 44 % Stotionary. 3 6 «Geminor. * 0 43 N.

30 4d «Tauri

ebm or i
2346 Yind Q Stationary.
21940 hdc --- B2398
3410 3d¢ - y 4508. DECEMBER.
$3 - $d eGeminor. * 1 43N.[—a 2» mw
$1631 96€ --- 25208] & 646 Pd
7110 h6O 21319 ¥s
7 4 - Gd FScorpi * 1 e8N.] 51446 WS
11 10 29 greatest elong. 46 51 E.] 5 14 52 & greatest Hel, Lat. N, ]
112346 Hd¢ --- W35GN] 11 118 F greatestelong. 21 10 W.}
12 0 - 96 eScorpli * 0208.) 12 8 5t Pink
12 7 3 Y in Aphelion. MWo323 USE +++ YON,
13.23 - Qo wScorpii * 0468.]15 - - Ceclip, vis ot Greenwich.
17 2 3 Q greatest Hel. Lat. 8. 7 isdt Sd --- J 042N,
2t 326 ude --- XO 14S. | 1815 - PS pSagit. * O43 NL
2293 - hd OVirginis * 0 325,] 21 348 PinInt dO < i
23.23 - $6 dGeminor. * 1 10S] 2t 18 30 Oentere 4. Winter comm*
2323 4 gd --- $1255, ]841090 RSE --- ke 68.
25 7 - 2dAOph *O4AYN.) 283 FSC --+ PORN,
30 BIS hdd --- hesis|221i0 Pde --- 2 4aaN.
Zn
S69 --- ¥Yaars,

476 SATURN'S RING, 1834,

ELEMENTS FOR DETERMINING THE GEOCENTRIC POSITION,|
MAGNITUDE, AND APPEARANCE OF SATURN'S RING.

Mean Noo. Pp om a u : v
fag = 8 4 40°29 4+6'07 + 8 39°8 + é 1 4
Feb. 10 3 86 43°06 6°33 827° 6 368
Mar, 22 3234 44°57 5°68 715-4 721
May 1 34nn 43-72 4°36 5 59°6 7469
June 10 347°8 41-20 405 | 5384 8 216
July 20 3 39°0 38°49 4°34 6 28°83 855°9 °
Aug. 29 31770 36 62 5-23 8122 9 29°9
Oct. 8 2 47°0 35°98 6°43 10 18°1 lo 36
Nov. 17 215°6 36°69 7°78 12 143 10 36°9
Dec. 27 151°3 38°66 9-04 13 31°5 Nn 99
Sh | —149°6 38-92 +915 $13 36°1 | +L 13-2

p.... denotes the inclination of the Northern semi-minor axis of the Ring to the,
circle of Declination; + East, — West.
@,.. the major axis of the Ring. :
b... the minor axis; + North surface visible,
— South surface visible.
1... the elevation of the Earth above the plane of the Ring, as seen from
Saturn; + North, — South,
U,,. the elevation of the Sun above the plane of the Ring, as seen from Saturn;
+ North, — South.
‘These Elements are founded upon the following determinations of
Brssex and Struve.
Let & represent the mean Longitude of the Ring’s ascending Node, at the time ¢.
i, its mean inclination to the Ecliptic.
a, the major axis of the Ring at the planet's mean distance.
Then, & = 166° 50’ 41” + 40”-65 (¢— 1800)
fees sees aa ULE paar (21890) } (Astron. Jahr. 1829, p. 175.)
40-098 (Astron. Nach, N° 139, p. 392.)

PHASES, 1834.° 477

Aprarent Disc.

‘The Moon's Libration is here supposed ta
take place in the plane of her Orbit:—and by
the time of the greatest Libration of her Ap-
parent Disc is to be understood the instant at
which, to an observer at the centre of the
Earth, the variation of the Disc from its mean

state has attained its maximum.

ereozza2Zann

‘The right-hand column indicates the qua-
drant of the Moon's Disc in which the Li-
bration takes place, and in which the greatest
change of the Moon's surface will become
visible.

PAweZor
MENSNSM sn ehehananehenaengm<

Ss.
8.
s.
8.
Ss.
8.

TABLE,

Snowine Taz Ictumnxatep rortion or TRE Discs oF Venus AnD Mars.

‘The numbers given in this Table represent
the versed sines of the illuminated portion of
the Discs, the Diameters of the Planets being
considered as unity.

TIDES, 1834,

MEAN TIME OF HIGH WATER AT LONDON BRIDGE,
Reckoning from Noon of each Day.

ocrOBER,

a
2
s
ajo 1
o]0 2
6}r 3
qe 3
sis 4
g}3 5 1817 43
wo}4 6 718 25 i
ufs 64319 2] 1
216 7
7 8
8 9
9 V
0 27
1 234
0 3 315 18
0 3 3515 54
1 4 1016 30
2 4 5017 16
3 54018 9)
4 6 3si9 10
4 7 47/20 26
; de
5
6
i

Example:—Required the Mean Time of High Water, at London Bridge, for the
eae of Jan, 13, 1834,

ite the day preceding, viz. 12, and, in the 2nd column,
1 1" ion Pernt being dimi by 12” gives 4* 10" for toe of of ‘ilgh ie
in a Esher

date, and in the Ixt column, under January, fe 4* 31",
which is not High Water in the Afternoon.

or HIGH WATER, ox tax FULL CHANGE or rmx MOON,
AT THE UxpEn! Pours axn Piaces,

England - - 1 eal eae -~ + + Engl
W.C,oF Scotland 11 45) Plymouth Dock Yard England ~
English Channel 6 0 Portland Race- = England -
River Thames = 12 England -
Scotland -

= 3 45| Portsmouth Dock Yd. England -

Rahn ChurehBayN. C. of Trek 9
Ramsgate Harbour
Rye Harbour = -

Sultees- = + -
Scarborough = ~
Scilly Islands ~~

Selsen Harbour
‘Shonnon Mouth

pomerers

England
France - Shields -

Skerries -
Sligo Bay =
Ireland ~ Solebay — -
River Thames - 11 30|Southampton
Bristol Channel - 6 45|Spithead -
Spurn Point
St. Ives -
‘St. Malo

Sue Saem dso ta upset
dia tiaatane soe tees
Siat oS ene ve anieS isis

= + England
- River Thames - 2

LoughCarinetord Ireland Ei

&
England Waterford Harbour

Werford Harbour -
Ie of Wight Weymouth = -
England Whitty - - -
Wales - - Wicklow - - -
France - - Wisbeach = = =
River Thames -12 30|Wranger Ooz = =

Roelsna ‘Yarmouth Rouds -
ete Yarmouth Sands =
Yorkshire Coast ~
var Youghalt = - =

TABLES. 483

TABLES FOR DETERMINING THE LATITUDE BY OBSERVATIONS
OF THE POLE STAR OUT OF THE MERIDIAN.

TABLE I.
Containing the First Correction,
Argument :—Sidereal Time of Observation,

paeeal Correction,
‘Time,
ton ° ”
oo J|—131iz 4
10 132 12
20 133 1
30 133 39
40 134 7
50 1 34 24
10 1 34 30
10 1 34 25
20 1 34 10
30 133 44
40 133
50 13219
20 131 21
10 1 30 13
20 1.28 54
30 1 27 25
40 1 25 46"
50 1 93 57
30 1 21 59
10 119 51
20 117 34
30 115 8
40 112 34
50 1 9 52
40 171
10 143
20 1 057
30 0 57 45
40 0 54 26
50 051 0
50 0 47 29
10 0 43 53
20 0 40:11
30 0 36 25
40 0 32 35
50 0 28 41
6 0 |—o 48 +

= mh 8

5 s2agssassara=e”

Tees ossoooscccoscosococoses
Aecorenaragseases! es

BSSSSs2255
eeseocoessococsescoccesss

*peg*eggacason

tee ene men ascss

cone

3 =
s-sehhonsercsaagannneses4

Pedansaas sac ecoocococoses

ite Le
“sseessoeoesosossoooscssesesooos

PR oconme nce nocnmomencruna
MESR2 2a aan t2zeze

~seccoecosssoeecoccosseococss
=

TABLE Uf.

Containing the Third Correction, (always to be added).

rooo-tmenaoae me ennoaneean

meeeccosscecoscoesoesosessoss

Arguments :—Sidereal Time and Date,

Feseconnamenoconnoonamnans

T“eeescoecceosoocaescocseooss

*"eecoceossesesescococoesose

Soe)

meocessoecoceesooesooesoos

Fesesososssoscecsososcooge

Ase a ee heh OmM te OD ar)

Arguments ;—Sidereal Time and Approximate Latitude.

i
i
i
}
2

<2 5 a eed

Serle momnaonsrrcer som noosa
TRS lSISV Sas ea” sSeasat

Tees sccocnmmamannmamnaeHmoss
Fae cea eam ene rane errs CFE
a TASMHS*GSlet ear Va sas
CARAS 6 REE SA

Taasanazomeouomemmsnseeren
PeSUMasgrRenr-Scan

ee ee

nen ecnsso- maone
“SoS Gre gcesessenseanasoRs

Tesco ose oC Om Re RR eerncosco]e

ae ee 2 ee
SRSLSSOHRRRTLLSSR AIS

Tece oes oso SHH RH osoescss

See came oaaoseenererasaasen
SSHRSRORSATANSSRRRA

eeese ses ec os seen en escoscess

ee eee eee
2aeSf8 RPSRRTS

tecsosessoccon-H-Hescessoce

ee ee ee ee es
Daas sSe5Saassann=

Tso scooooosooosScoSpSeSsooScSoS

.
ee >scecscs°s°s°ececgeegca=
foe ant we OS NR Dn

TABLE It.
Containing the Third Correction, (always to be added).

Arguments :—Siderenl Time and Date.

=
-

i
qe
‘ay
5
6
ri
38
9

Enis

S88 S88 £88
See SSe 288

0712033

0713036
0'14038
015041

o 16044
0°17047
018049

o-ngose
0 20055
021057

022060
0 23063.
0124066

025068
026071
027074

091085
0 32088
053090

0 -s4098
035096
0 36099

o-371o1
0 '38108
039107

040110
OMe
OMSLIS

OASIS
O-aizo
O451e8

0746126
o-47129
049131

O-49134
0*50137
0-51140

ose142
O°53145
054148

O*s515T
036153
07156

°

078214

079216
ow0219
O-wigee

Os2225
0 "83227
0 84230

o-91z49
o-gesse
093255

04257

‘Sidereal Time at the preceding Mean Noon - the Equivalent to (he giver Mean Time.

Examein—To convert 2 22” 254-62 Mean Time at Groanwich, Jan. 2, 1934, into Sidereal Tume.

‘This Tanxe is useful for the convervion of Musx Sotse into Smmmeat, Time,

‘Sidereal Time requiced

‘Sidereal Int
‘The Sum Is the Sidercal Time required, 21 9 23-04

} ‘The Table gives the

2 0" OF
oO
35

O62

‘Sidereal Time at the preveding Mean Noon, vit. January 2 =

38) 270453)

12 57 52°2157
18 57 42°3862)
14 57 32°5566)

1557 22"7270)
% 57 12°8975|
17: 573-0679)

18 56 sB7ea84
19 56 4374088
20 36 33°9792!

21 56 23°7497
22 56 13'9201
23.36 470906)

A 52°9555
43-92°9917
44:52°6278

45 524640)
46 s2-s002

47 5271364

48 51°9725
49 51°8087
50 516449)

51 SU4810
52 513172
53 511534

97 50°4981
58 50"3343

60. |59 5071704

Cen coe wee

32 234 233

=

see

4

‘Sidoreal Noon, wit. --- ==
‘The Sum is the Moan Time required, J

om OF
90
3
004

’ ‘This Tanta is useful for the conversion of Suoxmess, info Mean Sotaw Times
‘Mean Solar Time required = Mean Time at the preceding Sidereal Noon -. the Equivalent to the gives Sidereal Time.

‘Mean Time at the

Examrra.—To couvert 215 9% 23-04 Sideroal Time at Greenwich, Jan, 2, 1834, inte Mean Time,
For Sidereal
Tutervols.
:

LATITUDES AND LONGITUDES OF THE PRINCIPAL

OBSERVATORIES.

Gitlingen -
Greenwich -
Kensington
Kew ~ =
} Konigsberg
Lisbon = =
Madras
}) Monheim

Morecilles
Marlin - - |

Latitude, | Tangitude, Pliee. Latitude, Longitude.
oe sm ow dh om
+57 856/40 823 |Milan- -|445 28 2|— 096 46%6
460/87 OVE 8. 9 Modena -|444 38 35|— 0 43 41

453 32 51 |—0 39 466] Montpelier | +43 36 16|— 0 15 31
+54 21 15 |4+0 26 30 | Montauban |444 0 55\—0 5 23

Moscow -|455 45 45|— 2 30 12
452 848 —0 249 |Munich -|448 8 20/— 0 46 26°5
+52 31 45 |—0 53 35-6)
+52 524/40 1 3 [Naples -!44050 15\— 0 57 9
+53 4 38 |—0 35 156] Nicolet - +4658 55|\- 2 8 14
+47 29 44. |—1 16 10
+51 37 44/40 121 [Osforl -)451 45 40/40 5 0
+36 32 0/4025 10 | Padun- -|445 24 2/— 6 47
+52 12 53/—0 0 28:5] Palermo -| +38 6 44\— 6 5%
3356 3 |—1 13 55-8 alla |—33 48 45/10 4 3.
+50 350 )/—1 19 49-6] Poris - -|+4850 4/— 0 9 216
Pavia - =) 445 10 one me
+58 20 47|—1 46.55 | Pekin - -| 499 54 18 (BG
+55 23 13 |40 25 14 | Peteesburgh |+59 56 28 11s
Portamouth |450 48 3/4 0 4 24
+55 56 42}40 3249 | Progue -|450 5 18|— 0 57 42
#43 46 42 |—0 45 3-6) St, Helena |—15 55 27/4 0 Bi :
St.Fernando! +36 27 45/4 0 24
+46 12 0 |—0 24 38 | Slough -|451 30 20/4 0 *e
$50 56 8 |—0 42 56 |S.Kilworth | 452 25 ity
+51 31 50 |—0 39 46 6) Spires - -| +449 18 55|— 0 33 46
+51 28 40 o 0 0
‘Tubingen - | 448 31 10|— 0 36 ta
+51 30 12 )40 0 46'8)Turn - -|445 4 0/0 30 42
+51 28.37/40 1 3 7
+5442 12 |—1 22 0:6) Uraniburgh | 455 54 38 |/— 0 50 52
$38 4224/4036 34 | Veronn -| +45 26 yao 4 1
Vienna = - | 4-48 12 3 1 531
$18 4 8|—5 21 11 | Vivier -| 449 29 19/= 0 18 5a
449 29 18 |—0 33 5h
#4317 49 |=-0 21.29 | Wilna- -|454 41 2/1 41 10
+43 54 28 [0 42 18

North Latitudes and West Longitudes are indicated by the sign 4 2”
South Latitudes and Lest Longitudes by the sign —,

- 491

EXPLANATION OF THE ARTICLES
~~

. CONTAINED EX
THE NAUTICAL ALMANAC AND ASTRONOMICAL EPHEMERIS,
v=

FOR THE YEAR 1834,

+
- ‘

Abt the articles of tho Ephemeris have been comyuted for Greenwich MEAN solar
| time; and where they are expressed for apparent solar or sidereal time, it has been
|| Ghielly for the convenience of astronomers. A day is the interval of time between the
I ‘of any meridian from a heavenly body and its succeeding return to it, and
its name from the body with which the motion of the meridian is ‘The
between the departure and return of 4 meridian to the Sun is called a solar
r (salen adele ag ie fetches
_ & Aidereat day. ‘The revolution of the arth on its axis it always performed in the
| same time; and if the heavenly bodies preserved the same positions with respect to
i est oy ey el gh no ae hy

‘same, and all days, consequently, of equal length. ‘The Sun, (or, more strictly,

‘fn its orbit,) the Moon, and the Planets are, however, in continual motion 5

oan ‘yelocitics not only different from each other, but varying in each particular
ees of a day, as determined by any of these boilies, is therefore a variable

~ Astronomers, with the view of obtaining 2 convenient and uniform measure of
ety ete to a mean solar day, the length 9 i ae
oF nll the it solar days in 2 year. An imaginary Sun, ealléd the mean
| Beas erect Si inord vaitraly ta (he Bauitor wid Wie Weal Bis feron Ne
| fm Right Ascension, and tho interval between the departure of any meridian from the
mem! Sun and its succeeding return to it is the duration of the mean solar day,
‘Clocks ane Chronometers are adjusted to mean solar time; #0 that a complete revolution
(through 24 hours) of the hour hand of one of these machines should be performed in
‘exnetly the same interval as the revolution of the Earth on its axis with respect to the
meen Suh. If the mean Suh could be observed on the meridian at the instant that
‘the eloek or chronometer indicated 0° 0 o*, it would again be observed there when
the hour hend returned to the same position, As the time deduced from obterya-
‘tions of the true Sun fx called trve or apporent time, so the time deduced from the
gean Sun, or indicated by the machines which represent it, is denominated mea
time.

“We ennnot immediately obtain mean time from observation; but, from an obser
vation of the true Sun, with the nid of the equation of time, which is the angular
distance in time between the mean and the trae Sun, we may readily deduce it,

the true Sun to be obeerved on the meridian of Greenwich, Jan. 1, 18345
i ‘then be apparent noon at that place; the equation of time at, that instant
| $* 49°40, und, by the precept at the head of the column, it is “ fo be adided fo api

492 EXPLANATION.

parent time," hence it appears that the corresponding mean time is 0* 3" 49°40, oF

that the mean Sun had pnssed the meridian previously to the true Sun, and that at

an ee arene mean time clock or chronometer ought to indicate
tine,

‘A mere inspection of the columns of the Ephemeris is, of inet sien area |
that the quantities are continually varying, and that some reduction is necessary |
where data are to be obtained for any time differing from that for which the
quantities arc: registered, Take, for inatance, the Sun’s Right Aceutie 2 el
bf the month of January; on January 1, it is 18° 46" 26°79; on
is 18" 50" 5160; in the course of 24 mean hours it has Heap
4° 24°61, If, then, the Right Ascension were required for any ete
Mean Noons of January 1 and 2, ns at 6° from Mean Noon of Jutuaty 1, \srodla be
necessary to increase the Right Ascension on January 1, by the proportional part of
the daily increase duc for the 6%, viz, by one-fourth part, or 1" 620. This would
in all cases be required, even under the meridian of Greenwich, for which the i
have been specially computed. Let a person be now supposed to be under a meridian:
15° West of Greenwich, ‘The potitions of the heavenly bodies, as referred to the centre
of the Earth, are independent of meridinns, and are the same for all places at the
ame absolute instant; but the relative times at Greenwich and the assumed meridian
‘would be different, If i¢ were 1 from mean noon at the one place, it could not be a*
from inean noon at the other; for when we speak of time, we mean, as regards a
visible phenomenon, the distance of the Sun weshward from a given meridian, and at
the same absolute moment of time the Sun cannot be at the same distance (reckoning
westward) from two meridians which arc 15° distant from ench other, Before we can
make use of the Ephemeris, it is therefore necessary to ascertain, in every instance, the
distance of the Sun (in time) from the meridian of Greenwich, or what is commonly
called the corresponding Greenwich time; and this is evidently equal to the given time
under the assumed meridian, increased or diminished by the difference Cin time) of the
two meridians, accordingly na the assumed meridian is to the Westward or Eastward of
Greenwich. In 4 mean Solar day, or 24 mean Solar hours, the Barth, by its rotation
from Weet to East, has caused every meridian in succession from East to West to pars
the mean Sun; and since the motion js uniform, all the meridians distant from each
other 15° will have passed the mean Sun, at intervals of onc mean hour; the meridian to
the Eastward passing first, or being, us compared with the Sun, always one mean hour
in advance of the Westerly meridian, When it is 6‘ from mean noon at a place 15°
Weat of Greenwich, it is therefore 7*from mean noon at Greenwich; and it is for this
Greenwich time that we must deduce the quantities required feom the

Ifa chronometer adjusted to Greenwich mean time be at band, the Greenwich time
muy be immediately obtained by applying a correetion,sdeduced from the rate and
interval clapsed, and this will be preferable in all cates for obtaining the requisite data
from the Ephemeris,

‘The day adopted in this Ephemeris is supposed to begin at mean noon, or at the
instant when a clock or chronometer shows 0° 0" 0", Greenwich mean time, and ia
continued through the 24 hours, to the following mean noon, when another day begins.
At may therefore be called the Mean Astronomicad Day; although, in practice, astrouo-
mers always begin the day at the snoment that the Sun’s centre is on their meridian,

Jn the civil, or common, method of reckoning, the day is supposed to commence at
the preceding midnight, and to be counted only to 12 hours or noon, when the 12 hours
are reckoned over agnin to the next midnight. The civil reckoning is therefore always
12" in advance of the mean astronomicul reckoning; and the civil time corresponding

ii x — = a

P EXPLANATION, 493

to any given mean astronomical time ix henco readily found by adding 12 to the latter:
thus, if to Jan. 1*7"49", mean astronomical time, be wided 12", the sum will bo
Jan. 1 19*49", or Jan. 1° 749% P.M. civil time. Again, to Jan. 1* 15".35%, mean
‘astronomical time, add 12°; the sum will be Jan, 2" 3" 35" A.M, civil time. Tt,
‘thus appears that, from noon to midnight, the day of the month and the hour of the
day are the same in both methods; but from midnight to noon they differ; for at mid=
‘sight, when a new civil day commences, the mean astronomical day wants 12" of its

of civil into mean astronomical time is on the contrary performed by
Herein ts fee oy 12. ‘Thus, January 2 3" 35° A.M. civil time, diminished,
by 12%, Ieaves January 1" 15" 35° for the corresponding mean astronomical time,

To each month there are devoted twenty-two pages, distinguished” by the Roman
from 1. to XXII.

For the convenience of taking out differences, the quantities that follow next im onter
of succession have beet inserted at the bottom of each page. ‘Thus the quantities
opposite to Febroary 1 will be found inserted also opposite to Jamunry $2, the num-
er of the days in cach month having been intentionally increased for such purpose,
~ Page 1. of ench Month.

s contents of this page are adapted to Apparent Noon, or the instant when the
-centre ison the meridian of Greenwich. The Sun's Right Ascension, here given,
with Aberration, and reckoned from the true Equinox; it is therefore the

at Apparent Noon, or the time which ought to be shown by « Sideroal

at that instant, ‘The Sun's Declination, at Apparent Noon, is the apparené

F listance of the Sun from the Equator, measured on the meridian,

_ ‘The columns entitled “ Diff. for t hour”? are intended to facilitate the reduetion of
‘the quantities from the meridian of Greenwich to any other meridian, The values of
these quantities for any propoeed mean time will, however, be more accurntely ascertained.

of the numbers on page I, from which, indeed, they have been derived.
Skdireal Time of the Sun's Semidiamoter pasting the Meridian is wsefil for
redecing a transit observation of either limb of the Sun, when one only has been
observed, to the transit of the centre.

‘The Equation of Time is the difference between Apparent and Mean Time, and
therefore seryes for the conversion of either time into the other. The numbers here
given, show, for Greenwich Apparent Noon, the distance of the mean Sun from the
‘meridian, or the portion of time to be added to, or subtracted from, (according to the
‘precept at the head of the column) Greenwich Apparent Noon to obtain the corre

fig Mean Time at the same meridian, or the time which ought to be shown by

¢ Menu Time Clock. It differs from the Equation of Time in page IT,, becanre
the equation itself vorics in the interval between Apparent and Mean Noon, If
‘we turn to page I. of the month of April, we observe, at the head of the column,

a site © which signifies that achange of precept occurs in the course of the month:

and between the equations opposite to the 15th and 16th days of the month, a black
Tine, indicating that the change occurs between the Mean Noons of those days. The
upper precept is to be applied to all the quantities ubove the black line; be rs
Tower precept to all the quantities below it: that is, in. the instance referred to, the

of Time fs to be added to Apparent Time from the Ist of April to the
instant at which the equation becomes 0" 0', which happeus between the nouns of the

PXPLANATION.
Ainys of the month ut after that instant the equation i to be

zs
E
z

i
i
i
E
ip
e

time
time; to convert it into mean tise, the equation of time is
{it f to be applied to apparent time, according to the precept at the hes

the apparent time deduced from an obvervation of the Sun om

1834, in longitnde 45° or 3° east of Greenwich, to be 6, and po 2
to convert it inte mean time : Sabiracting te ditrenc of ng 8 fm

the apparent time at the place, we have 3” for the

Greenwich. ‘The difference of the equation for 1 hour is O"S41, cat

3, gives 2523 for the variation in 3 hours, Soe

rif

Gut
Ha

tion is increasing) to 10" 4*-41, the equation of time at aj
10" 6°93, to be added (acconling to the recent t tbr ed arate
Lig ‘apparent time 6", wheuce we obtain 6° 10" 6"93 for the mean

. Page II, of each Month,
‘The Sun's Right Asconsion and Declination at mean noon bre bon dodol rom

ity Iongitude and latitude given at page IIL, and the apparene

ecliptic at p. 266. ‘They denote the sis ent hen of Af Ge ea ge
to the equater, und the true equinox, at the instant the Greenwich mean tiny
@lock, or chronometer, indicates 0° 0 0", or when ts honey capa 96S oR
¢qual to the equation of time,

‘To find the Right Ascension and Declination for any other mean time and
at 920" A.M. March 2, 1934, in longitude 98°, or 6” 32" weet of
astronomical time, corresponding to 9* 20 A.M. March 2, is 21" 20" from the noon
of March 1, or March 1° 21" 20", agreeably to what has been said before, "The lon-
gitnde, ‘West of Greenwich, must be adied to March 1* 21" 20", and the reeult,
March 24'9* 52", is he corresponding Greenwich mean time, for which the Right
Ascension and Declination are to be found. ‘The difference betwoen the Right Ascen-
sions on March 2 and March $ is 3" 43°91, that is in the 24 mean hours succeeding
the Mean Noon of March , the Right Aeccnsion bns increased by that rer
it will, Deeb Lee recat © perpen pert Oe CAN Tncretes Sea
Amount fs readily obtained by thia proportion; 24”: 3* 49*94-: 3° 52": 360s;

‘being added to 22" 31m 3749, the Right Ascent Mean Noo of Mar %
gives 22° 52° 13°97 for the Right Ascension at the time

Jn a similar manner the Declinations indicate a decrease of 22” rijaaat an
hours; therefore 24" : ge” 555 +: a 52": 3! 416, the proy Pie Re
decrease for 3° 52", wich, mtriied fps 8.40 98 1°0, Lan BPA 4 for
the Declination required,

The Semidiameter of the Sun. ‘The riumbers in this column express the angle at
the contre of the earth subtended by the Sun's Semidinmeter, and they are required for
reducing observations of the limb to the centre, as in the instance of measuring
‘tude of the Sun's upper or lower limb, or the distance of the Moon from the Sua.

ion of Time. The numbers in this column are the valuca of the equation
at the instant of Mean Noon, and therefore serve more particularly to convert Afean
inte Apparent ‘Time: for this purpowe we have ouly to edd the equation where the pre=
cept directs it to be subsracted, and subtract where it is directed to be added, Thus, if

aE ail

EXPLANATION. 495
See 96 cen Nave of Ape 1, be subtracted the equation 4” 106, the aif

0 getela corresponding apparent time. ‘To find the equation of time
on April 15, 1834, in longitude 62%, or 4° 8 West of Greenwich.
‘Ada the difference of longitucle to the” given time, because it in west, and the corre
mean time at Greenwich ie April 157" 8", ‘The variation in

\ 34 hours is 14°87, that js the sem of the equations belonging to the uous of the
because the equation has decreased to 0, and then increased in the

2a: 4872: Se wag,
greator than 0" 4°°31, the equation onthe 1548, which was docreasing,
See Fe in passed through its state of decrease to zero,
)now increasing. The difference 0*11 ts the equation of time at the time
2 re ne toe than et de

Time at Moan Noon is the angular distance of the First point of Aries, or the
tue Vernal Equinox from the meridian, at the instant of Mean Noon: it is therefore
the Right Ascension of the Mean Sun; or the time which ought to be shown by a

‘Clock at Greenwich, when the Mean Time Clock indicates 0 0" O',
A ‘Clock nenesexrs the rotation of the Earth on its exis, as referred to the
8 ear performing a complete revolution through the 24 hours im the
internal between the departure of any meridian from a Star and its next return to it.
‘At the moment that the Equinox, or a Star whose Right Ascension is 0” 0% 0°, ie on
the meridian of Greenwich, the Sidereal Clock ought to show 0° 0™ 0%, and at the
‘Teturn of the Star, or the Equinox, to the same meridian, the Clock ought

Sneten Ge time,
time hore intended is that in common use among Astronomers, and
expresses the actual hour-angle from the meridian, westward, of the true equinoctinl
pout at the moment of observation. It is. therefore affected by the equation of the
equinoxes ; and is not, strictly speaking, a mean or wuiforvaly increasing quantity. Lt
pe Saha to be termed apparent sidereal time in the same manner 48 apparent
ereckone from the actual arrival of the sun's centre on the meridian ; and in
us mean solar time ia reckoned from the arrival of an imaginary sm,
with its mean velocity, so mean sidereal time (whose expression

ould bo simply O°* 6% Jorge) youd be rockoned from the trasit of (not the

True, but) the mean equinoctial point. ‘The smallnees of the fluctuations to which a
“ sparent sidereal time compares, with one regulated tw mean wide~
Jy iiss beng at the utmost only #*3 in a period of nineteen years, has
the practical inconvenience of this from being felt: no clock being suffi-
perfect to go during xo long & period without frequent restdjusting ; mud as
‘the corrections applied by astronomers to the observed right ascensions of all objects
are. to this supposed irregularity in the rate of the clock, the mean right ascen-
ions cords out correct, It has, therefore, not bees thought necessary, in
this instance, to depart from teeeived usage, however theoretically objectionable such
wode of counting time may appear, since a change in this respeot would involve the

+ OF m corregponding change in all tables of mutation.
time at Mean Noon is useful in all cases where mean solar time ix to

Wiens from observations of the heavenly bodies.

) werres to facilitate the reduction of siderea) to mean solar time, and nce
toms y the help of the tables commonly uscd for that purpose, called a Table of c=

496 EXPLANATION.

celerntion of Sidereal on Mean Solar Time, and the corresponding Tsble of Retardation
of Mean on Sidereal Time, according to the following rule:—Convert the interval
from the mean noon immediately preceding, from the denomination given, to that
required ; and if mean time be required, the result will nt once be that which the clock
should show; bat if sidereal fine bu that png the. neni ad: Pasa
sidereal time at the preceding mean noon,

Example :—To convert 21* 9" 23'-04 sidereal time, Jan. 2, 1884, into mean solar
time, for the meridian at Greenwich,

Sidereal time given - - - + = = + = === at Sebo
Sidereal time a mean noon, January ®@ ~ = = = = 18 4634702

Interval in sidereal time from mean noon= + =~ = 2 99 4908

Retardation of mean on widereal time for the interval = — 2340
‘Mean solar time required - - - - - > - = - 2 22 25 62

which is the interval elapsed since mean noon, expressed in mean time; and there-
fore the time which ought to be shown by a mean time clock.
Vice versd, to convert 2 22" 25°62 mean solar time, January 2, 1834, into
nidereal time for the same meridian.
‘Mean interval from mean noon, January 2 - - = = 292 95:62
Acceleration of sidereal on mean time for the interval = + 23-40

Sidereal interval from mean noon ~ = = = = = - 222 49°08
Sidereal time af mean noon, January 2 - - - - - 18 46 34°08
Sidereal time required’ - - - - - - = = = - 21 9 2304

‘which ought to be the time shown by the sidereal clock at the instant in question.

If the place of observation be not on the meridian of Greenwich, the sidereal time
must be corrected by the addition of 9'8565 for each hour (and proportional parts
for the minutes and seconds) of longitude if the place be to the weat of Greenwich ;
but by its subiraction, if to the cast, Thus, in 9" 10™ 6° weat Tongitude, the sidereal
time at mean noon, Januury 2, Instend of being, as in the Example,
18" 46” 34° -02, must be corrected by adding 1" 90*-37, thus giving 18” 48™ 4°99
for the time to be used, instead of that set down in the column.

‘The conversion of mean solar ‘to sidereal time, and vice versa, muy, however, be

and with perhape less liability to error, by meana of this and of the golumn
entitled Mean Time of Transit of the First point of Aries,” at page XXII. of each
month, using the Tables of Time Equivalents, ‘inserted at pages 496 to 459,

To convert menu solar to sidereal time: To the siderenl time at the proceding
‘mean noon add the equivalent sidereal interval corresponding to the given mean time;
the sum will be the sidereal time required. (See Exainple at page 487.)

‘To convert widereal to menn solar time; To the mean time at the preceding
sidereal noon, add the equivalent mean interval corresponding to the given sidereal
time, the sum will be the mean solar time required. —(See Example nt page 489,)_

‘This mode of reduction is adopted by Professor Anvr, in preference to the former
method by means of Tables of Acceleration and Retardation, and it possesses the ad~
‘vantage, that there is no distinction of caves, and all the quantities are wlditive, ‘The
‘Tables of Tine Equivalents differ from the Tables of Acceloration and Retardation, in

at —

EXPLANATION. A0T

puters.
itital ine atne nso we in fating Ge mun tine of can of «

Page TIT of cach month.
The Sun's Longitude, bore given, é« affected with aberration, and reckoned from the
true equinox: it is therefore the apparent longitude of the Sun at the inatant of mean
‘noon; ar it js Cif p denote the Radius Vector) the true longitude of the Sun at the
tine: 775 p, because aberration causes the Sun to appear behind its true place

in the

‘The Sun’s Latitude ix the angular distance of the Sun's centre from the plane of
the! ‘measured on a circle perpendicular to that plane,

‘The La of the Radius Vector of the Earth is the logarithm of the distance

between the centre of the Barth and the apparent place of the centre of the Sun at mean
fog the mean distance, or the semi-axie major of the orbit being considered unity.
‘These quantities are derived immediately from the Solar tables, and enter into,
indeed are the foundation of, nearly all the subsequent operations in the
Whenever the true longitude of the Enrth is required, as in calculating the Geo
‘centric position of a Planct or Comet from its Heliocentric porition, it is necessary to
meduee the apparent longitude of the Sun to the true, by correcting it for aberration.
The Suv’s aberration for every tenth day is given at page 266, and may thence
be readily obtained for any other day of the year. (See Aberration, page 508.)
In strietness, the Logarithm of the Radius Vector should also be corrected for aberra-
tion, but this is generally neglected, the correction being too small to affect the accu~
my of the results in practice,
‘The Sun's longitude, entering into the expressions for aberration and Solar nutation,
is required for the reduction of the Stars’ placca,
‘Phe Moon's Semidiameter is Che angle under which her Semidiameter would appear
if viewed from the centre of the Earth; and her Horizontal Parallax is the greatest
¢ under which the Earth's Equatorial Semidiameter would appear if seen from
‘centre of the Moon. ‘The former is requisite to obtain the position of the centre
from an observation of the Moon’s limb, us in all cases of altitudes or lunar dis-
fances. The latter, for computing the horizontal purallax of the Moon at any given
latitude on the Earth, considered as a Spheroid ; also for finding the parallax in alti-
Right Ascension, &e., for the purpose of reducing, an observation of the Moon
m the surface of the Earth, to what it would have been if made at the centre.
observations of the Moon made at sea, the horizontal equatorial parallax
iigeaealy et for finding the parallax i in altitude, without regarding the Sib
reduction to the Spheroid; but in calculations requiring considerable preci¢ion, as in
Junar oecultations and solar eclipsey this reduction cannot be dispensed with.

‘To find the Moon’s Semidiameter and Horizontal Parallax at 6” A.M.
enemy 7, 1884, at w place 15°, or 1° to the eastward of Greenwich. ‘The civil time
At the place, expressed in mean astronomical time, is January 16* 18", from which sub-
tencting 1", because the place isto the eastward of Greenwich, we have January 16" 17"
for the corresponding time at Greenwich, or 5" afier midnight. Proteeding from the
semidiameter given for midnight, we must compute the proportional part of the varia~
tion in oes the time elapsed since midnight, viz, 5"; and a aay

EXPLANATION.

Purposes at nox, it will suffice simply to take this proportional part for the Correction
ef the registered valoe the given time: thus the eemidiameter, for mide
iy et alae is 14! 484, and for the 17th at neom, or 24's it is
SU"1; the difference 27 is the variation in 12 hours, Therefore — -

1g: 2%7: 258: 1125, :

which, added (because the quantities are increasing) to 14" 48"4, gives 14" 49S for
the Moon's Semidiameter at the time propored. Siadkchy, the Heel aaa
midnight of the 16th is 54 20"3; and at the noon of the 17th it ix 54’ 3071;
the difference 98 is the variation in the 12 hours, which include the givest time ;
Harare, 198 Sa P2400, or 41, whith axed Coos Ul pee
to 54’ 20", gives $4' 244 for the Horizontal Parallax i

greater accuracy be desired, a further correction must be applied to the

2 14 54S

‘The mean of the second differences is 0°75, and 4 of this, which is the grealest effect,
is very tently equal to 0” “1. -

The Moon's Longitude and Latitude at Mean Noon and Midnight indieste the

Noon and Midnight, it is necessary to apply the equation of second, and sometimes

‘even of third differences, on account of the irregular variation of her motion.

‘The Moon's Age at Mean Noon is the Mean Time elapsed since the Moon's ecliptic
conjunction with the Sun, or since the Son and Moon had the same Longitnde, The
numbers in this column represent her age at Greenwich, and are expressed in days, and.
decimal parts of a day. :

‘The Moon*s Meridian Passoge —This column contains the Greenwieh Mean Time,
to the nearest tenth of a minute, at which the Moon's centre is on the spper Meridian
of Greenwich, nnd is useful to indicate when the Latitude may be obtairted fret ae
observed meridian altitude of the Moon ; also, &t conjunction with the Semi-diurmal

4‘ 4

EXPLANATION. 499

the times of the rising amd setting of the Moon : bebaientdach
of High Water,
bol (db) denoting conjunetion occurs, as on Junumry 9, we st6 10
1 that the Moon does not pass the upper meridian on that day at Greenwich:
‘the exse once in every Junation, and arises from the circumstance of the Luiar
mig greater than the Mean Solar day, and inchiding it within its limits, In the
piawiasce, the exces ig.69%°8, or the loner day in equal to 24" 52"'8 Mean
the Moon passes the meridian on the Sth at 23° 43"°9, or 16"-1
tn of he sma ne ers 99
¢ ofthe 10th. For the same reason there is also one day in every luna=
| ‘the Moon does not transit. the lower ineridinn, and this happens about
‘opporition, or when the difference of longitude of the Sun and Moon ix
. In the list of Moon-culminating Stars, at pages 416 to. 453, the days on which
me transit occurs are readily scen. On January 9th (page 416), for instance, it
that the Moon transits only the lower meridian, while on the 24th (page
‘only transit is that at the upper meridian,
‘Mean ‘Time of ‘Transit under any other Meridian, suppoxe 45° or 3" weet
of! on January 15, 1834. The Meridian being to the west of Greenwich,
the Transit will take place after the Greenwich time of ‘Transit on the 15th; there
fore take the difference between the Meridian Passages on the 13th and 16th, which
in 40-7. ‘Then, 24": 40"-7 : * i
alla gives 4" 298 for the Mean Time of Transit at the given

Would avo taken place befure the Transit at Greenwich, axd the proportional part tha
|) ifererce, vin, "1, rast in thie cnse have been subtracted. "The times thus deduced
Jeeta sy wn ecient seen ir he epsom

— Pages V to XIE of each Month,

Mosn? é Right Ascension and Declination for every hour of the day, with
agent ad 10 minutes, By means of the quantities here we th
(pepe Moon's rising and setting, &e., may be deduced, with

early ns little labour oe ie required in the ease of the Sur, ‘The numbers represent
‘of the Moon, as it would appear from the centre of the Earth, with respect
Equator and the true Equinox: and the tre giveti for every hotir, witli
the view of refidering any correction for second differences unm , except where
extreme precision is required. The Right Asceneion for any tite ta readily obtained by
simply adding the proportional part of the hourly variation due to the interval elapsed
wince the preceding hour. Thus, suppose the Right Ascension af the Moon were
1 hd ttaead time of January 8, in longitude 60°, or 4° enst of Green:
Wick, ‘The given time, 8" 45, diminished by 4%, gives the corresponding Greenwich
#45". The Right Ascension at 4° ia ei 12 275, md ot 5° it is 18° 14"
the difference, 2° 20°17, fx the Increase in the interval, or 60%. Hence,
60% 2 2017; 45" = 1" 45°13, which being added to the Right Ascetsion at 4°,
gives 18° 15 for the Right Ascension at 4” 45° at Greenwich, or at 8” 45
wider the sstumed meridian. To find the Declination, we make use of the ntim-
bers in the column healed * Diff. Dec, for 10"7* ‘The number in thie coltimn stand-
fig opposite to nny hour is } of the difference of the Declinations at that and
the following hour. We therefore say, 10"; 2227: ; 45": 1002, which Being”

2x3

00, EXPLANATION:

Sg Cees ch estate a terested) 8/275 Cea Sa
» ives 5.23° 9’ 41/6 for the Declination at the time proposed.

‘The Phases of the Moon, ‘These are given at page XII, to the wearest tenth of a
‘mimate. The numbers denote the Greenwich Mean Time, at which the differences -
of Longitude between the Sun and the Moon are 6, 90°, 180°, ar 270% being

0? at the New Moon,
90° at the First Quarter,
180° at the Full Moon,
270° at the Last Quarter.

‘The Moon's Apogee and Periger. The numbers here given indicate, to the nearest «
hour, the Greenwich Mcan Time at which the Moon is respectively at her greatest and
Teast distance from the Earth. .

Pages XIIT to XVIIE of each Month.

Lunar Distances—These pages contain, for every third hour of Greenwich Mean ~
‘Time, the angular distances between the centres of the Moon and certain heavenly
bodies, such as they would appear to un observer at the centre of the Earth When «
Lunar Distance has been observed ou the surface of the Earth, and reduced tothe
centre, by clearing it of the effects of parallax and refraction, the numbers in there
pages enable us to ascertain the éxact Greenwich mean time at whiely the objects would
have the same distance. They are arranged, from west to eas, commencing cach
day with the object which is at the greatesydistance acestiard of the Moon, in the
puecise order in which they appear in the heavens; W. indicating that the object ix
west, and E, east, of the Moon. Thus we have at one view, by a aimple reference to
the date, all the lunar distances which wre available for the determination of the

le.

‘The columns headed “P.L.. of diff” contain the Proportional Logarithms of the
Differences of the distances at intervals of three hours, which are used in finding the
Greenwich time corresponding ton given distance, according to the following rule, ¥iz.;
Seck in the Ephemeris for the neares( distance preceding the given distance, and take
the difference between it and the given distance; fran the proportional logarithm of
thie difference subtract the proportional logarithin standing opposite to the searest
distance in the Ephemeris; the remainder will be the proportional logarithm of a
partion of time to be added to the hour answering to the nearest distance, to obtain
the approximate Greenwich mean time corresponding to the given distahec.

If the distances between the Moon and nv Star increased or decrensed uniformly,
the Greenwich time, corresponding to a given distance as found by the above rule,
would be strictly correct; but an inspection of the columns of the Proportional
‘Logarithms in the Fphanate will show that this is not the case; and as the know-

of the exact Greenwich time is indiepeneuble, a correction must be applied. to
the time #0 found for the variation of the differences of the distances. This correction
may be obtained by means of the Table at pnge 482 of the present volume, in the |
manner:—

1. Find the Approximate interval, by the preceding rule...

2, Take the difference between the Proportional logarithms standing opposite to the
distances in the Ephemeris which include the given distance.

8. With the approximate interval and this.differeace a9 arguments, take out the
correction from the table.

i

EXPLANATION, BOL
t decreasing, add the correction to the approximate
i a ila live trinsic

| ete were required to find the Greenwich Mean ‘Time, at which

‘between the Moon and x Aquila: would be 54° 54" 16” on March 29,

aed bby inspecting the distances, that the thme must be between III”
"; therefore take the

Distanee at LIL” = 39 2957 and PL. - = 3549
True Distance ~ 54 54 16

Difference - 035 41 ---P.L, - - 702s
Approximate Interval 1'20"48*~ ~ - PLL, = = 8479

‘The difference between the Proportional rithms in the Ephemeris, at 11" and
VI" is 72. Opposite to 1" 20", and eta the Table, we have for the correc-
subtracted from the Approximate Interval, 1% 20" 48%, because the
‘Logirithms are increasing, gives 1" 20" 26° for the truc interval from

= Bence the Greenwich Mean ‘Time ie 4” 20" 26".
In the present instance, we vee that the omission of this correction would ptoduce
‘an error of 5/80” in the Longitude. It is, however, an extreme case; for & Aquilae
distant from the Moon's path than the other objects used for Lamar
5 but the distance has here been taken near the limits, or when the Moon's
so towards the object is such as to render the observation table

Beiter logarithms also verve to point out the object which is most
circumstance for accurate observation; that object being. to be pres
ferred which has the least Proportional Logarithm opposite to it: for, the greater the
velocity of the Moon from or towards a Star, the greater ia the reliance to be placed
fon an observation of the distance; and it is a property of Popes ee
‘ecrease ae their natural numbers increase; a smaller Proportional
fore, indicates u greater velocity of the Moon, or a greater variation of Sais ta Oe
‘Wsterval, upon which the value of the observation depends. ‘Thus, on January ty 1834,
between Noon und It", Pollux is the most eligible star, because the
Logarithm, 2294, is less than those of any which follow it; and, by inspecting
the columns of Proportional Logarithms, it will appear to deserve the preference
throughout the 24 hours of the Ist day; though at XXI", from the Moon's motion
during the day, it is evident that Regulus is gradually getting into a better position ;
‘and ifwe look to VI" on January 2, we shall sec that it has really the advantage over
Pollux nt this time.

On the Ist day of January, between Noon and [1T*, the following is the order of
‘preference as indicated by the Proportional Logarithms, viz. Pollux, Antares, Regulus,
‘Mars, Sun, Venus; between III” and VI" Regulus would haye the preference of An~
tures, because the proportional logarithm of the difference is lees, and the order of the
others would remain the same,

Te is by no means to be inferred from these remarks that observations of any of the
Wistances are to be neglected; on the contrary, every registered. object should inva-
miably be observed when an opportunity offers. If, however, on a comparison of
‘Feauilis a considerable difference should be diacoversl, the Proportional Logarithms
Will indicate the objects less liable than others to be affected by errors of observation,

Le

EXPLANATION,

bz
fad Sates tvering 9 greater degree of gutcpney-os tn tba nemmeyif-A)

Page XIX of each Month,

Configurations of the Satellites of Jupiter,
In addition to the explanation given at the foot of the pas it may B

Intitudes, but merely to distinguish them in their relation of upper and Lower.
‘Phe Satellites gre in the puperior parts of their orbite, or haye Jupiter between —
them and the Earth, when they are moving towards the right hand of th but
they ure in the inferior parts of their orbits, or between the Earth | jupiter,
when they are moving towards the left hand.
‘Ifo telescope that inyerte be directed towards Jupiter on March 15, 1834, at 8*
‘Mean Time, the Satellites will appear to an observer at Greenwich in the positions a

EF.
i
a
“ij
'E
HE
3
ie
=

right.
geo West" and Apparent East,” at the head of the page, sve inserted to
show the positions of the Satellites with respect to Jupiter, as they would appear im
& telescope that doce not invert, Jupiter being always to the South of the genith of

pb alegre ora ae pepe merely, the pnge viewed direetly, exe
‘Dibile tho Satellites in an'inyerted onder; but if the leaf be turned over, and the page

position of a Satellite from apparent to real, or vice rorsm,
de to draw a Fee de canis Lontck Teeter en ac
this

upon line at the sume distance from the centre as before, only on the oppesite
wile. If this ion be the Configurations as laid down in this
‘vollame, the Satellites will be exhibited in thelr real positions.

iluy following, according to the common mode of reckoning time; that is, the Confie
gurations ué 14” on August the Ist relate to 2” A.M, on August the 2nd. 2

‘Phe Configurations ennble ap observer to distinguish the Sutellites from each other,
gnd from Stare in the vieinity of Jupiter.

Page XX of each Month,
Ectipses of the Satellites of Jupiter.
this page are given the Mean and Sidereal Times of the Eclipses of the Satellites,
ss

exhibiting the position of each Satellite with respect to
the at the moment of tmmersion Bonin, a vil Ba

, — —
eS 4 —— i SS |

which are even within these limits have been also eal os) mds Rs
‘such eclipses have been sometimes observed.

: im.) denote the instant of the disappenrance of the Satellite, by
entering into the shadow of Jupiter; and the Emersions (Em.), the instant of its re-

‘at coming out of the shadow. ‘They generally happen when the Satellite is

some distance from the body of Jupiter, except near the opposition of
ter to the Sun, when the eclipse takes place near the body of the planet. ‘Before

the Immersions and Emersions happen on the West side, but after
‘on the East side of the planet: With an inverting telescope the appears
‘be directly the contrary. Before the opposition, the Eumersions only of the
are visible; and after the opposition, the Emersions only. It is seldom,
» that the Immersion and Emersion of the xecond Satellite can be observed at the
+ but both the phenomena are generally visible with the third and fourth

To find the time at which the Immersion or Emersion of any of the Satellites will
take place under any other meridian than that of Groonwich, it is merely necessary to
odd the erence of of longitude (in time) to the time of the phenomenon at Greens
|, if the meridian be cast of Greenwich, or to subtraet it if it be west, and the
or difference will be the time required, But this determines only the instant of
‘occurrence of the phenomenon, Jupiter ify be below the horizon at this time 5
‘or he may be above it, und the intensity of sun-light, or even the brightness of the
such as to render the Satellites invisible. To have the Eclipses visible,
‘it has generally been considered that the Sun should be nt least 8° below the horizon,
end Jupiter not less than 8° above it at the same time, Adopting these limits, 4e is
‘then necessary to ascertain the position of the Sun and Jupiter, with respect to the
‘at the time of the phenomenon. ‘This may be readily accomplished by
meana of # celestial globe, or near enough fui tha pooyaue: Vy Badiag tha Neate
‘tising and setting of the objects, with the assistance of a table of semidiurnal area,
The Eclipees of Jupiter's Satellites, especially of the firet, afford us, perhaps, the
‘adiert means of determining the longitude; all that is necessary to be known
the exact time of observation: the difference between this time and the time at Greens
‘Wich, shows the difference of longitude at once, and it is east or wert of Greenwich,
according as the time of observation is greater or ese than the Greenwich time.
‘Suppose the Emersion of Jupiter's first Satellite to be observed, on January 2, 1834,
at Paris at 19* 53" 557 Mean Time at that place; by reference to page XX, it
appears that the Emersion will take place at the Greenwich meridian at 19° 44" 34°E
Mean Time; the difference, 9" 21"-6, ia the difference of longitude between Green-
wich and Paris; and, because the Paris time is greater than that at Greenwich, we
Pe et Exc ig to the eastward of Greenwich,
ee is the tables, there are difficulties in the observation of
ee unfit them for accurate determinations of longitude, exeept an
een Vi oper pryaninns. Ditlerent telescopes give different trent
‘thould be taken to have recourse to those Ppebptetodel ia peach di |

=

a

EXPLANATION. 505
eee given are the ete eee, pers hicks
abi ath the method weomnanatel fy Pama Beak iy tar ha

for Mean Midnight at Greenwich, according to the formula exhibited at
$71, omitting in © and D the term depending on 2 €

Si cncacguss ler pier wales op tmanreceestagines

‘Where, however, the apparent place of any Star, not in the Astronomical Society's
, is requited, similar quantities to those must either be computed with refer-
to each particular Star, before we can use the A,B,C, D, or recourse must be
to other and independent means; such, for instance, as are afforded by the Tuble
Pages $72 und $73, which serves equally for all Stars. ‘The construction of this
"Table is explained at page 371.

‘The following Examples will suficientyiustrate the mode of using both the Tables,
the Comection (A a) of the Right Ascension and (3) of the Declination of

_-y Orionis (No. 648, Ast. Soc. Cat.), for Preceasion, Aberration, and Nutation, at
Greenwich Mean Midnight, on February 5, 1834,

1,—By the Astronomical Society's Constants and the Logarithms of A,B, CD.

bio ow
‘Mean m Jon.1, 1830----516 100 Moan 3------=-- + em IT0
Your Years Precession

‘Mean «, Jan. 1, 1834 -

ee eee a

+ 5°3130
«+ blade

= FMT es ee 0887

D ---~ 49-6890
aD 2. + 618205

# « Now Tables for facilitating the Computation of Precesion, Aberration, and Nutation of 2881
Privcipol Fixed Stary, together with a Catalogue of the same, reduced to January 1, 1830, Computed
ai the Expense and vunder the Direction of the Astronomical Society of Loudon, To which is prefixed
oe juction explanatory of their Construction and Application. By Francis Baily, Esq. Loadon,
1827.

:

506 EXPLANATION.

‘2—By the independent Constants,
Fer February 5, 1834, the Table at pages 372, 373 faraishes

Bat Mes,

~ Oise ye 3g

ae $12898
eoo- - 49-9147
see 3 - - = + 0-0025 == sim = - 49-0329
+ LOB veer ee EU eT ee ory
— feet —
Ba (mare) = + 0-48
—_— Bene ~O-7716
Aa (in time) = 40°-082 cos 3 +9°9975
2 —0-7691 ---¢- — 5-88
7 bas
Hence the Apr. Right Ascems. of y Orionis = 5 16 13-64 +
‘And the Apparent Declination -------- r=+6 1 3839 —

2. Moan Time of Transit of the First Point of Aries.

The times in this column show the distance of the mean Sun from the meridian,
at the instant when the frue point of intersection of the ecliptic and equator (called
the first point of Aries) is on the meridian of Greenwich ; and as the distance of the
first point of Aries from the meridian, at the instant the mean Sun is on the meridian,
is denominated “Sidereal Time at Bean Noon,” this may, by analogy, be termed the
Mean Time at Sidereal Noon. It is the time which ought to be shown by a mean
time clock adjusted to the Greenwich meridian, at the moment that a clock, adjusted
to sidereal time, indicates exactly 0° 0" 0’ The use of this column is to facilitate the
reduction of sidereal to mean solar time, with the help of the Table of Time Equi
enta, given at pages 488, 489 of this volume, as has been already explained at
page 496, under ‘ Sidereal Time at Mean Noon.”

3. Mean Equinoctial Time.
Mean Equinoctial Time signifies the Mean Time clapeed since the instant of the
‘Mean Vernal Equinox. The numbers in these columns represent this time at every
Mean Néon in Mean Solar days, and fractional parts of a day ; they are reckoned from,

‘as the Equinoctial
pt 745186, it ix evident that the Equinoctial Year of 1833-4 was come
that a new year commenced, at 0497078 afler Mean Noon of the 22nd,
of the day at the head of the column is common to all the days of the
Thus, at Mean Noon of January 19, 1834, the Equinogtial
36, and on Janunry 20 it is 303°*745186, and so on until
078, when the yenr terminates, and the fractional part of the day
) Noon of March 23, 1834, the Equinoctial Time is 0° “505048, and this frac
‘be annexed to all the numbers in the column of days, from the period of the
‘until the equinox of 1835,
At the instant the Mean Sun arrives at the Mean Vernal Equinox, it must also be on
yoow caeridian, and this meridian will thon have its Equinoctial time
jt sn Solar ‘each of which will be 0” 0" 0', and they will continue to
throughout the Equinoctial Year. At the end of the Equinoctial Year,
have passed this meridian 865 bie toed ich jyeirmge
on of its 366th diurnal revolution, viz. 0° °242264 ; it will, therefore, have
‘some other meridian, which will now, in its turn, reckon the Mean Equir
d Mean Solar time from the same point, and remain constant for the year,
meridian from which the time is reckoned is shifting its position at the end
0* 242264, or 3° 48" 516 to the eastward. Between the Vernal
eq of 1834 and 1885 this “itinerant” meridian corresponds to Longitude
(3° °85 East of Greenwich,
‘species of time was first introduced in the Supplement to the Nautical Almanag
‘with 4 yery full explanation of its narare and use, [t there appears, that
‘of Equinoctial Time is to afford an uniform date, which shall be i
different meridians, and of all inequalities in the Sun’s motion, and shall thug
' ‘necessity, when speaking of the tine of any event's happening, of mentioning
Be re se glace wher it ves ober) or congue ‘Thus, it is the same
to ray that a comet passed its perihelion on January 5, 1834, at 5* 47" O'
Mean Time ot Greenwich ; at 5°56" 21'6, Mcan Time at Paris; or at 18337 288!
23" 40" 4°07 Equinoctial Time; but the former dates make the localities of Green~
wich and Paris enter ax elements of the expression ; whereas the latter exprestes the
‘period clapeed since an epoch common to all the world, and identifiable imdepend~
‘all logalities, By these means all ambiguities in the reckuning of time are
e Hed to be aynided,
eanvert Mean Solar into Equinoctial Time: To the carrespending Greenwich
Mego Time add the Equinoctial Timo at Mean Noon of the same day at Greenwich,
the sum will be the Equinoctial Time required, Thus, in the instance of the eomet
Hefore alluded to, Paris being 9" 21'-6 East of Greenwich, subtract this from the Paris

time and wo get 5°47" 0" for the corresponding Greenwich Time, to which add
186, or 285" 17° 59" 4"-07, the Mean Equinoctial Time at Grecnwioh Mean
January 5, and the eum will represent the Mean Equinoctial Time of the

of its perihelion, vig. 288" 25" 40" 4°07 from the yernal equinox of

elapsed since mean noon of Janvary 1, Moan noon of Janunry 1 is therefore reckon
0, and. 1 is foun opposite to thet of January 2, Vecauae a ie inte og ay
lapsed,

5, Fractions of the Yoar,

‘These fractions are the quotients found by dividing the numbers in tae
colums by 365-25. The days und fractions of the year ary upeful in
culeulations,

Obtiquity of the Ecléplic, (Page 266.)

‘The apparent inclination of the plane PE Det R AN ie here
given for every 10th day of the year, and continued to January 6 of the follaw=
ing year, marked December 37, for the ake of convent ‘This inclination
is ever varying, as well from the effect of its mean diminution, as of the nn-
tation of the carth’s axis: {It is on important clement in deducing the positions
of the heavenly bodies, with reference to either of the plancs, when we know
as with respect to the other; as, for instance, in computing Right

and Declinations from Longitudes and Latitudes, or vice vers, If the
‘apparent Obliquity be required for any date not to be found in the Table, it may
be obtained by simply taking the proportional part of the variation of the obli-
quity corresponding to the interval which comprises the given date. Thus, the my
rent Obliquity on March 6, 1834, is 28° 27' 39/41; for the variation of the
Quity for the ten days between March the 2nd and the 12th, is 0"13, or O"-O23 for
bme day, and this being wultiplicd by 4, the number of days between the &nd and the
6th, gives 005, to be added to the Obliquity of March the 2nd, For most purposes,
however, the Obliquity corresponding to the date in the Table nearest to the given
dato, is eullicient, as is evident from nn inapection of the quantities,

The Sun's Horizontal Parallax. (Page 266.)

‘The Sun's Horizontal Parallax is the grealest angle under whieh the equatorial
semidiameter of the carth would appear from the Sun's centre. It varies inversely
as the distance, and the numbers in this column represent the values of the Paral~
Tnx for every tenth day of the year.

‘The Parallax serves for reducing « Solar observation made at the surface of the earth
to what it would be if made at the centre.

The Suns Aberration, (Page 266.)

Tho progressive motion of light, combined with the motion of the Enrth in its orbit,
causes the Sun to appear in a different position from that which he really occupies,
the truc position being always in advance of the apparent. The numbers in this
column indicate, for every 10th day of the year, the umount of aberration, or the
quantity to be applied to the dru longitudes of the Sun to obtain the apparent

SS

EXPLANATION. 509°

longitudes. - The longitudes derived from the Solar Tables include Aberration, and are
therefore apparent longitudes, such as are contained in this Ephemeris. If the true
longitude of the Sun be wanted, as is the case in finding the longitude of the Earth
for the calculation of the Geocentric place of a body, the aberration must be applied
with a contrary sign.- Thus, on June 10, 1834, at Mean Noon, by adding 20’"05,
the amount of aberration, to 79° 3’ 21/0, the apparent longitude of the Sun, we‘
obtain 79° 3! 41-05 for its true longitude. -

Equation of the Equinozes. (Page 266.)

‘The Solar and Planetary Tables furnish us with the places of the Heavenly Bodies
referred to the Mean Equinox ; but the true place of the Equinox at any time differs
from its mean place, by a quantity which is termed the Equation of the Equinoxes ;
and the numbers here given show the value of the Equation for every 10th day of
the year. They are to be applied, with their proper signs, to the Longitudes, reckoned
from the Mean Equinox, to obtain the values with respect to the True Equinox :

If the Longitude of a body be given with reference to the true Equinox, this
Ephemeris, and it be required to find its Longitude reckoned from the Mean Equinox,
the Equation of the Equinoxes must be applied with a contrary sign. Thus, the
longitude of the Sun, reckoned from the true Equinox, on July 10, 1834, at Mean
Noon, is 107° 40’ 201, and the Equation of the Equinoxes is — 16-47; therefore, °
applying it with the contrary sign, the sum 107° 40’ 36-57 is the Sun’s Longitude *
frem the Mean Equinox on that day.

‘The Equation corresponding to any date not found in the Table, may be obtained
in-the usual way by interpolation.

‘The Equation of the Equinoxes in Right Ascension in a similar manner enables us
to find the apparent point of intersection of the Ecliptic on the Equator ; and is neces-
sary in computing Sidereal Time.

Mean Longitude of ('s ascending Node. (Page 266.)

‘The numbers in this column are the Mean Longitudes of the Moon’s ascending
Node, at Mean Noon of every 10th day of the year, reckoned from the Mean Equinox.
‘The place for any intermediate day is easily found from the daily motion inserted
‘at the foot of the column. The Longitude of the Node is necessary in the calculation
of Nutation; it is also used to determine roughly the Stars which are likely to
undergo occultation by the Moon.

Ephemeris of the Planets. (Pages 267 to 361.)

These pages contain the Geocentric and Heliocentric Places of the Planets, Mer-
cury, Venus, Mars, Vesta, Juno, Pallas, Ceres, Jupiter, Saturn, and the Georgian.

‘The Geocentric Places are the places of the centres of the planets, as they would
appear if seen from the centre of the Earth; the Heliocentric, such as they would
appear from the centre of the Sun.

The positions of the larger planets are given for Greenwich Mean Noon of every day
in the year. But those of the smaller Planets are given only for every fourth day,
except for the month preceding and following their opposition, when they are given
for Mean Midnight of each day.

610 EXPLANATION,

* ‘The Geocenitrio Right Ascension and Heliocentric
the True Equinox, ‘The Geocentrle positions are
therefore i

previously, to the Hoon of the 7th, viz, 11, as {0 want still 9 of ite
the termination of the 7th day. ‘The planetary day, ee
of February 7th it hegine befire the solar day nnd ends after i, aud eatindt

the metidion at any period of it.
Another phenomenon takes place in the ease of the planets, sets hehe aad
not occur with the Moon; it is that of two transits on the ¢ame day, which arises

ival of the following Mean Noon.

"The positions of the planets for any time not given in the Ej ino de
SES rye arte ape he ber
As an exaiple: Required Pali tye atsngpe oe tm fe
Mean Time of January 15, 1834, in longitude 30° weet of Greenwich; also the time of
Jupiter's passage over that meridian on the sme day. ‘The difference of longitude 2
Sa ea eet Hered ney iouy © $0 Cn any

at For the Right Ascension. The Right Ascension on January 15 is 1 40" —
and on Janunry 16 it i 1" 41" 13''88; the difference 19°08 ix be riation of the
Right Ascension in 24 mean shoure; therefore, 24° ; 19°08 : > 636, the

Proportional part of the variation anewering to 8"; and thie peered part added
Tinian the Right Ascension are increasing) to 40” 54°80, the Right Ascension
‘ft mean noon on January 15, gives 1" 41" 116 for the Right Ascension ri a

2. For the Dortination. Declination on January 15 is Ng? 1971

‘om the 16th it is N.9° £5" 25''6, the difference, 2! 7/0, in the varintion in 24

and the proportional part of this vatintion for 8* ix 42’"6, which, added to tie De-

clination at noon on the 15th, gives N. 4? 14! 08 for the Dectination

ohne deans ‘Take the difference of the times of to consecutive
transite, coneldering this difference av an acceleration of retartation of the Meridian

Pastaze while the planet las passed over 24” of loruitude; and take the

part of it, due to the difference of meridians, for a correction to be to the

Meridian Passage at Grecawich, bearing in mind thef in enst longltades the passage

_

EXPLANATION. 6il

ptecedes that at Greenwich, when times are accelerated; and follows it, when they are
retarded ; and the contrary in west longitudes. In the present case Jupiter passes the
tmeridian of Greenwich on January 15 at 6" 271, and on January 16 at 5" 585;

the difference is 3"-6, therefore 24": 3"-6 :: 2* : 0-3, the proportional part to be sub-
tracted from 6" 2"°1, (because the passages are retarded, and the longitude is west of
Greenwich) which gives 6* 1"8', mean time at the given place, for the Meridian Pas-
sage. Where great accuracy is not required, as in predicting the time of passage, in
order to be prepared for observing the altitude of the planet on the meridian, for the
determination of latitude, this method will suffice.

Parallaxes and Semidiameters. (Pages 359 to 361.)

These are given for the noon of every 5th day of the year, and may casily be inter-
polated, if required for any proposed day, by simple proportion.

The “ Equat. Hor. Par.” represents the grealest angle at the planet, subtended by
the equatorial semidiameter of the earth. It serves to find the Parallax in Altitude,
Right Ascension, &c., for reducing an observation at the surface to the centre of the
earth.

The Equatorial Semidiameters represent the angle subtended at the centre of the
earth by the Equatorial Semidiameters of the planets. They serve to reduce an obser-
vation of the limb to the centre, where only one limb of the planet has been observed

Fized Stars. (Pages 362 to 415.)

In these pages is given every particular relating to 100 principal fixed Stars. The
contents of the Catalogue for January 1, 1830, (pages 362 to 367), are sufficiently
explained at pages 366, 367, as are also those of the Catalogue for January 1, 1834,
at page 370. Next (page 371) follow Brssex’s formule of reduction, and (pages
372 and 373) « table for the Reduction of Stars, independent of the Astronomical
Society’s Catalogue, an example of which is given at page 506,

‘The apparent places of « and $ Urse Minoris, are given for every day of the
year, and those of the remaining 98 Stars for every fenth day. They indicate the
positions which ought to be shown by perfect instruments at the time of their transit
over the meridian of Greenwich; and, therefore, supposing the catalogue of mean
places to be correct, they serve to detect any errors of the instruments.

‘The hours and minutes of Right Ascension, and the degrees and minutes of
Declination, are placed at the heads of the columns as constants, and belong
equally to all the numbers below them. This arrangement has rendered it necessary,
in numerous instances, to continue the seconds beyond 60, as the width of the page
would not permit of otherwise indicating any change in the minute. Thus, the ap-
parent Right Ascension of « Gemrnonum at page 389, on October 8, 1834, is registered
J" 23" 61''45, and is to be read 7*24"1"45. Again, the Declination of 6 Centauri
(page 397), on July 10, is registered S. 59° 33’ 85"-31, which signifies S. 59° 34’

25/31. Also (page 387) the Right Ascension of 51 (Hev.) Cephei on December 7 is
6* 19° 125*-39, and must be read 6 21™ 5°39,
‘The stnall figures on the right hand of the vertical colutnns of séconds tepresent the

the interval. Thus, at page 385, we find in the instance of 6 Taunt, an
posite the interval between June 10 and 20, and a difference of 017 opposite to

interval between the seconds belonging to those dates ; we therefore infer that 11 transits
have taken place, and that the daily variation of the Right Ascension is 0"-015. |

‘The Mean places of the 160 Stars have not been all equally well determined.
are now introduced for the first time, whose places can only be considered nx
mately known, It has, therefore, been deemed expedient to ‘the!

Sture, that is, the Stars whose places may be relied upon, by small capitals, aa ATAcar
and 3 Onioxts, at page 385.

Aya general rule, it is good to preserve all quantities given at certain intervals ina |
state fit for interpolation by simple proportion. ‘This rule tae |
case of the apparent places of 3 Stars near the Poles of the Equator, which, |
treme accuracy is required, demand » further correction, depending on the term which
involves 2. (Series ar paged.) ‘The apparent placee do not inéhide thete
corrections, on account of the rapid variation of the argument, viz. about 26° in a day,
but they are given in a Table at pnges 414, 415, for every degree of the Moon's Longi-
tude, and may be readily applied, agreeably to the precept at the foot of that Table,

Moon-Culrinating Stars. (Pages 416 to 453.)

Thote Stare have been denominated Moon-Culminaring Stars, which being nénr the
Moon’s parallel of Declination, and not differing much ftom her in peer
‘fase proper to be observed with the Moon, in order to determine differences of
diane. This is effected by comparing the differences of the Sinan HiuC ASS
of such a Star and the Moon’s bright limb at any two meridians. Ef the Moon Kad to
motion, the difference of her Right Ascension from that of a Star would be constant at
all meridians, but in the interval of her transit over two different meridians, her Right
Ascension will have varied, and the difference between the two compared
will exhibit the amount of this variation, which, added to the difference of the
diane, shows the angle through which the westerly meridian must revolve before | it
comes up with the Moon; hence, and knowing the rate of her increase in Right
Ascension, the difference of longitude ia easily obtained.

For the determination of this variation, recourse has hitherto been had to actual
observutions male at different meridisns, because any errors in the computed places of
the Moon and Stare ore thereby avoided ; and the places given in previous Moon-
Culminating Lists have been given merely with the view of indicating the times when
the observations are to be made, Tn the present List, however, the Right Ascensions
have been given with every posible degree of accurncy, so that they may be con-
sidered, ut least approsimately, in the light of corresponding observations made at
Grecawich, and be taken to represent the actual indications of the Greenwich
instruments, the same as though they had been already observed, The traveller has

ob |

EXPLANATION, 513
dering his observations immediately available for determining

‘of the Moon’s bright limb are given for cvery day, with a view

accurate determination of its variation when required. The Moon’s age

‘upper transit, to the nearest tenth of a day, is inserted in a pa~
‘column containing the Magnitudes of the Stars.

rin the column ‘ Var. of ¢*e R.A. in 1 hour of Long.” represent the

‘im Right Ascension of the Moon's Limb during the interval of her transit

‘equidistant from that of Greenwich, and one hour distant from

have been deduced from the Right Ascensiona of the bright

therefore include the effect produced by the change of the scmidiameter,

determine the Longitude where the difference of meridians is not very

the difference is considerble, and extreme accuracy is wanted, that

‘Thus: Multiply the difference of longitude between Greenwich and the
by the variation; aud, accordingly as the given meridian is east or west
subtract or add the product to the Right Ascension at Greenwich ; the
it Ascension of the bright limb at transit over the given meridian : For
January 19, 1834, the Right Ascension of the Moon’s first limb is
52°35 at ite upper transit at Greenwich, and the variation for one hour of
longitutle is 125-38: Required the Right Aacension of the limb at its upper transit

‘at Paris. Paria 216, or 6, cast of Greenwich ; therefore, multi
2136 by 125738, and subtracting the product 1956 from 3" 6" 52-85, we have

9.6" 32°79 for the Rig cht Ascension at Paris.
Se icin teneratmivves aul x eet eee eee
to the object.

“Where an asterisk is placed opposite to a Star's name, it ix intended to denote that
‘the Star ia favourably situated for observing ita Declination along with that of the

Doth hemispheres, with a view to the accurate determination of the Moon's

numbers in the column entitled “ Sid. Time of (’s Sem, pass. mer," ex-
Sidereal interval which the Moon's Semidiameter, at the time of transit at
‘Greenwich, takes in passing the moridian, and therefore werve to determine the Right
Ascension of the centre from an observed Right Ascension of either limb,

Oceultations, (Pages 454 and 455.)

‘These pages contain a list of all Stars to the sixth magnitude inclusive, the
Occultations of which by the Moon will happen when the objects are above the
Hhorizon of Greenwich ; together with the Sidereal and Mean ‘Time of the Immersions
‘and Emersions, and the pointe on the circumference of the Moon’s disc, where the
‘Star, viewed with a telescope that invert, will disappear and reappear. By “ Angle
from N. Point,” is to be understood the arc included between the Star when in contact
and the point of intersection of the limb with a circle passing through the North Pole

3s Qu

_

54 EXPLANATION.

and the centre of the Moon; and by “ Angle from Vertex,'® the arc
‘eontect and the point where a circle, passing through the zenith and the
centre, intersects the limb; both as seen through an ‘an inverting telescope.

to the point of the Moon's limb where the Star will reappear, fm some in
Occultations have been inserted which, taking place in, or wear to, the
eka Fteentcehy se8 mt. siala therm bet maybe dade haere Pea aa

Elements for facititating the Computation of Occuitations of certain Stars by the Moon.
(Pages 456 to 468.)

‘The contents of these pages have already been briefly stated at page 468 The
numbers represent certain quantities which enter into the calculation of an Oceul- |
tation, bat pabediaterbapsiroetipteiee ses |
Earth, are independent of geographical position, and serve equally for all places. Ty
is only necesanry to apply the difference of longitude from Greenwich to the Green-
wich Mean Time of conjunction, to find the time of eonjuetion at any other meri~
dinn ; and it is this time to which the positions of the Moon and Star here given will

‘equally correspond,

‘Thus, the position of the Moon and @ Librar, on January 5, 1894, at 11" 48" 48%,
Mean Time at Greenwich, is the porition at 11" 58” 9" Mean ‘Time at Paris, because |
Paris is 9" 21%-6 enst of Greenwich.

By * Limiting Parallels are to be understood those parallels of latitude beyond
‘which an occultation cannot possibly be visible.

an observer situate at n star, and having the Moon between him and the

‘Barth, and that he could eee the Moon projected on the Barth's disc, he would sce
it moving across the disc from west to cast, covering a zone whose breadth would
‘be equal to the apparent diameter of the Moon, Now, it iv only within the limits
of this zone that the Occultation of a Star by the Moon can be visible, To all the
places through which the boundary lines pass, the Star will appear just to touch the
Moon's limb; and that projected parallel of Intitude, to which one of the boundary
eer a tangent, is one of the limiting parallel, while the intersection of the other
boundary line with the circumference of the Earth's disc, determines the other lmit~

ing parallel.

“Limi Parallels” are useful to indicate, without any further
whether at « given conjunction of a Star with the Moon, the positions are euch as to
produce an occultation in a given latitude, and thus to enve considerable labour to the
computer. Thus, suppose from the times of conjunction, at page 456, it were required
to prepare a list of occnltations for Greenwich, whose latitude is 51° 28/ 40” N.

On looking down the column of “ Limiting Parallels,” we reject at once the first
five state, becauee the Limiting Parallels do not comprise the parnilel of Greenwich.
On January 6, we see that y Ophiuchi will be ecculted co all the parallels of latitude
between 70°N. and 41°S., which include that of Greenwich; this Star would
therefore bo fixed upon for enleulation, if no dther considerations existed to cause
its rejection. We observe, however, that it is of the fifth magnitude, and that
the conjunction takes place near to noon: ‘The intensity of eun-light would therefore
Provent its being seen, and ic is rejected in consequence. ‘The next Limiting Parale

EXPLANATION. 515

Jela having Greenwich between them, are 62°N. and 6°S., opposite to 98 Scorpii, on
January 6 ; this star would therefore be selected. The time of conjunction in this
indtance, as regards sun-light, is not unfavourable: if, therefore, on further inquiry,
tha Star be found to be above the horizon of Greenwich, we should then commence
the calculation. It appears, on reference to January 6, page 454, that this occul-
tatien is visible at Greenwich,

Eelipses of the Sun and Moon. (Pages 469 ta 478.)

‘These pages contain all the particulars necessary for indicating the times, places, &e.,
om the Earth where these Phenomena will be visible; also the Elemente which bave
boon used in the calculations.

Phenomena. (Pages 473 to 475.)

Under this head are given the conjunctions in Right Ascension of the Planets with
the Moon, and with each other, and with certain Stars; also the times when the Planets
are in those parts of their orbits most favourable for observation, with a view to the more
accurate determination of their elements; and other notices, chiefly of use to the
astronomer.

Saturn's Ring. (Page 476.)

In this page are given the quantities which enable us ta determine the position of
the Ring of Saturn at intervals of 40 days throughout the year, and whether it be
sible or not. The values of p show the position of the minor axis of the Ring with
respect to a circle of declination, those of a and b the Ring’s apparent magnitude, and
@ comparison of those of / and J’ its visibility or otherwise. For the plane of the
‘Ring to be visible, it is necessary that the Sun and the Earth should be clevated on
the same side of it, which is the case during the whole of 1834. The circumstances
which determine the invisibility of the Ring are, 1st. when its plane passes through
the centre of the Sun, or J’ = 0; 2nd, when it passes through the centre of the
‘Barth, ov / = 0, and at this time bis also = 0; Srd, when the Sun and Earth are
on different sides of the plane of the Ring, for the Earth in thia case will have the
unilluminated side of the Ring turned towards it.

Phases. (Page 477.)

Fhis page contains two Tables, the first showing the Mean Time of the greatest
Libration of the Moon's Apparent ‘Disc; and the second, the [luminated portion of
the Dises of Venus and Mars at the middle of each month,

Tides. (Pages 478 to 481.)

‘The Mean Times of High Water at London Bridge are here given for every day of
the year, on the assumption that the time of high water at full and change days, or
the Establishment of the Port, is 9° 7, The first high tide which happens
after Mean Noon of any day is inserted in the Ist column, and the second in the
2nd column. Where a line (—) is inserted, it indicates that there ix only one high
tide on that day. Thus, on January 6, there is only one high tide: it occurs at
11°37, but the succeeding high tide does not take place until 7” after mean noon
of January 7.

‘The times of high water at full and change of the Moon, as given at pages 480 and
481, are reckoned from Apparent Noon: They represent the Establishments of the

. 2u2

516 EXPLANATION.

timer of High Water when the Mooi passes the meri
time as the Sun; or the intervals between the times of Transit

of the port at London Bridge, viz. 2" 7", and considering this as a constant quantity,
‘ing the difference of the tides between London Bridge and the several places, —
to be added to or subtracted from London Bridge tides, according a6 the extablish-

the estublithment of the port at Aberdeen is 0° 45", and at London Bridge 2” 7*;

the difference is 122", aud the Aberdeen tide precedes that at Loudon: therefore, by

substracting 1" 22" from the London Bridge tides, we obtain the Aberdecn tides in

mean time. On February 18, 1834, the first high water at London Bridge occurs at

8" 17", which being diminished by 1" 22", gives 6" 55" for the corresponding tide at
Aberdeen, and so of other places.

ishing th Corrente on ait of See renee a
the Greenwich Teme corresponding to a reduced Lunar Distance, (Page 48%.)
Eee neers eananiey Spa ee
Page 503,

Tables for determining the Latitude by Observations of the Pole Star out of the
Meridian. (Pages 483 to 485.)

‘These Tables serve to determine the Latitude from an observation of the Altitude
of the Pole Star out of the Meridian. The method of using them is us follows:

From the observed altitude, when corrected for the error of the instrument, refraction,
and dip of horizon, subtract 1’.

Reduce the Mean ‘Time of Observation at the place to the corresponding Side
real Timo, by the Table given at page 486, (See Tables of Time Equivalents,

517.)

Pith the Sidereal ‘Time found, take out the “ first correction,” with ite sigu.
If the sign be ++, the correction must be added to the reduced altitude ; but if it be
—, it must be subtracted : in cither case the result will give an Approximate Latitude.

With this Approximate Latitude and the Sidereal Time of observation, take out the
“€ second correction,” and with the day of the month and the same Sidereal time, take
out the “ third correction,” These two corrections, added to the Approximate Lati-
tude, will give the Latitude of the place.

Bxaurna.

On March 6, 1834, in Longitude 37°W. at 7" 43" 35° Mean Time, the altitude
of the Pole Star, when corrected for the error of the instrument, refmction, and dip
ha a6 a 28",

»
Dit Long 37? Sintiney = = ;
Greenwich Mean'Time = - 10

EXPLANATION. oy
Silereal Time ut Greenwich Mean Noon - atalsy
‘Mean Time at Place = = 7 43 35
‘Aeceleration (Table, p.486) for 10" 1a" — aL
Sidereal Time of Observation - - - 6 40 18
Correctod Altitude ~ - - ~ -4617'98"
Subtract She ee - 10
46 16 28
With Argument 6° 40" 13%, First Correction — 0 4 26
se
eS gon} Seam Correction 41 21

Arpanents Merch © 834: rand Ci <itiG
Yaiteas Mi the place = ~ 46 10 42
which agrees with an actual trigonometrical computation.

The Tables of Time Equivalents, given at pages 486 to 489, are useful for converting
Mean Time into Sidereal Time, and Sidereal into Mean Time, agreeably to the example
annexed to cach table, They will serve also for Tables of Acceleration aod Retarda-
“tion, by the difference between each argument and its equivalent, ‘Thus, in
‘the Table at pages 456 and 487, the e.ccess of the siderenl time equivalents above the
arguments of mean time ehow the acceleration of widereal on mean solar intervals ;
and in the Table at pages 488 and 489, the defect of the mean time equivalents, ax
compared with the arguments of sidereal time, indicate the retardation of mean on
‘sidereal intervals.

‘The concluding Table at page 190 contains the Latiludes and Longitudes of the prin-

Observatories. This Table will, iti hoped, be gradually perfected and com-

by communications, from cach astronomer, of the latest and most accurate
determinution of hie geographical position. -

518 ERRATA
IN THE NAWTICAL ALMANAC FOR 1834.

did et ae
Page 64, March 26, omit +2 on the right-hand of Jupiter.
Page 360 under Jupiter, for RAYS read ames

Page 495 line 18 - - - for nuruxsunts read represents

ERRATA, detected in the following Tables,

(Continued from p. xv, of the Supplement to the Nautical Almanac for 1833.)
I—Nouvelles Tables Astronomiques et Hydrographiques, Sc, Per V. Bacar.
Edition Stéréotype. Paris, 1829. to.

Paye 79 ab the top, for —L 2t*=5:36452 read —L 12*= 536452
BL PRO neeeeeees 950 = navevene 850

Table des Logarithmes des Sinus, Cosinur, $c.
Page 554 Sinus 89°58 47” for 8845 rend «BRAS
596 Cosinus 46° 32” 0” = =— 9960 — 9860

I1.—Tables Botiptiques des Satellites de Jupiter. Par M. Derawunx, Paris, 1817,

Premicr Satellite, Table 11, opporite to Avril, and under K, third line
from the
for 344 read 244

Second Satellite, opposite Arg. D 30, sixth line from the top,
for 20°8 read 20%
‘Troisitme Satellite, Table des Demi-Durées, last Differ, N ot
for 384 read 434
Quatritme Satellite, Perturbations for 1835,1, second line from the top, under
Difffrence, for 3°S read 3°0

IlL—Mathematicat Tables, §e, By Cusnixs Hurrox, LL.D, The 7k Edition,
by Ouray Gueoory, LL.D. London, 1830. Svo.

Page 6 Number 10282)

10966) ;

7 rogg7/ Mark over the 4th Bgure of the Log, is omitted.
8 —— 1149

10 —— 19385 for 392 read 1392
is —— 13968 — 342 — 342
13 13997 — 350 — 0350

284 Cotang. 9°24’ for 6°7919867 read 67719867

> —— v= at in|

ERRATA (continued), P 319

IV. Tabula Feneris, fe. Auctore Bexsuaxoo vp Lixpusat,
Gothw, spcecx. 4to,

Page VIE. Tabula IT. ¢ 1820 for 10° 16° 38! 46° read 10% 8° 58’ 46"
| under Aphelium, ise — 17 0" — = g®_ OF 20”

| -V—Inovetigatio Noea Orbite a Mercurio, &e, Auctow Brentanno ne Live
. vexav. Gothw, moccexrit. 4to,

[ables If and IIT, Pages V to EX, add 31” to each of the quantities in the column

; headed * Nou”

- For Table XIX. Page XL. substitute the annexed,

520

INDEX.

"4" The'large Roman Numerals indicate the Page of each Month ;
the small, the Page of the Preface; and the Arabic, the Page of the Book.

Abbreviations and Symbols - = *
Astronomical Society's Report - -
Calendar, Principal Articles of -
Ceres, Ephemeris of - - - - -
—————— for Opposition

Configurations of the Satellites of Jupiter

Day of the Year - - - - -
Eclipses of Jupiter's Satellites - -
the Sun and Moon -
Equation of Time - - - - -
the Equinoctial Points

Equinoctial Time - - - - -
Explanation - - - - - - -

Festivals and Anniversaries - - -
Fraction of the Year - - - -
Georgian, Ephemerisof - - -
Juno, Ephemeris of - - - - -
————— for Opposition -
Jupiter, Ephemeris of - - - -
Jupiter's Satellites, Eclipses of - -

Occultations, &c.,

Law Terms and Returns - - -
Lunar Distances- - - - - -

Correction for Second Difference of

Mars, Ephemerisof- - - - -
—— Phasesof- - - - - -

Mean Time of Transit of the first point of Aries

Mercury, Ephemeris of - - - -
Moon-Culminating Stars - - -
Moon, Ephemerisof - - - -

—— Libratio of - - - - -

Phases of, Apogee and Perigee -

Pages
+ xiv
xii to wai
- xxii
318 to 320
321 to 322

469 to 472
Tand II
- 266
- XXII

518 to 519

491 to 517
- XXII

347 to 358

308 to 310

311 to 312

323 to 334
- XX
- XXI

- xiv

XIII to XVII

- 482
291 to 302
- 477
- XXII
267 to 278
416 to 453
III to XII
- xl
- 477

Moon, Eclipses of -
Moon's Node, Mean Longitude of - - - - - -
Obliquity of the Ecliptic - - - -°- - - -
Observatories, Longitude and Latitude of the principal

Occultations of Fixed Stars by the Moon, visible at Greenwich

Elements of

of Jupiter's Satellites by Jupiter - - -
Pallas, Ephemerisof - - - - - - - - =
———— for Opposition - -
Parollaxes of the Planets - - - - - - = -
Phenomena - - - - - - = - = = = -
Pole Star, Tables to find the Latitude by - - - -
Report, Astronomical Society's - - - - - - =
1830- - - - - -
1834- - - - -

Stars, Mean Places of, for{

—— Apparent Places of, 1834- - - - - -
— Constants, for Reduction of - - - - - -
—— Logarithms, for Reduction of - - - - -
— Formule, for Reduction of - - - - - -
Correction of, for2€ - - - - = = =

Saturn, Ephemerisof - - - - - = - = -
Ringof- - - - - - - - - - -
Sidereal Time at Mean Noon - - - - - - -
Semidiameters of the Planets - - - - - - -
Sun, Ephemeris of - - - - - - = - = =
Eclipses ofthe- = - - - - - - = -
—Abermtion of - - - = - - =: =
Parallax of - -

‘Time Equivalents, Tables of - - - - - - -
Transits of Jupiter's Satellites and their Shadows -
University Terms - - - - = - - = - -
Venus, Ephemerisof - - - - - - - - -
Phasesof - - - - - - - = + -
Vesta, Ephemerisof - - - - - - - = -
———_———— tor Opposition - - - - -

- 490
454 to 455
456 to 468
- XXI
313 to 315,
316 to 317
359 to 361
469 to 475
483 to 485
xii to xxii
362 to 367
368 to 370
37440 418
372 to 373
- Xx
- 371
414 to 415
335 to 346
- 476
-
359 to 361
Ito II

478 to 481
486 to 489
- XXI
- xiv
279 to 290
- 477
303 to 305,
306 to 307

LONDON:
Printed by WILLIAM CLOWES,
‘Dube Street, Lambeth.